Southern African Large Telescope
Proposal Information for SALT Call for Proposals:
2018 Semester 1
Phase 1 Deadline: 31 January 2018, 16:00 UT
SALT Ast Ops
20 December 2017
Petri Vaisanen and Encarni Romero Colmenero
(Ast Ops Managers)
This document provides information to potential SALT proposers that will assist in making their Phase 1 & 2 proposals for 2018 Semester 1 (1 May 2018 – 31 October 2018). It summarizes the essential features for new users, the latest instrument status, and changes from previous semesters. It incorporates the latest experiences from SALT Astronomy Operations regarding telescope and instrument performance. The instrument simulator tools have been updated to reflect the current situation. The document also includes proposal policies and related information. The SALT website should be consulted from time to time for further updates. The Phase 1 proposal deadline is 31 January 2018 at 16:00 UT. The Phase 2 proposal deadline is 13 April 2018 at 16:00 UT.
Table of Contents
This document is organised as follows. Sections 1 – 3 form the introduction to SALT and describe the proposal process. Sections 4 – 10 cover the details on the telescope and instrument characteristics. The appendix gives a glossary, a list of the SALT partners, and technical details on the instruments.
For recurrent users, the most interesting sections will be the status of the current semester, including a list of changes from the last call, presented in Sec 1.3. In addition, each instrument section gives the specific current status for that instrument at the beginning of the relevant section (6.1 to 9.1). At the end of each instrument section the current Calibration Plan is given. Important dates and deadlines can be found in Sec. 1.5. The version of the PIPT and the related tools are the same as for the 2017-2 semester, but there will be a new release of the PIPT for the Phase 2 submissions (see Sec. 1.6). It is also advisable to re-familiarise yourself with the details on the proposal submission (Sec. 3) and to make note on important information (given in bold font).
If you are a recurrent user but have not applied for time lately, you can refresh your memory browsing the tips presented in Sec 1.2 and the relevant telescope and instrument performance sections for any news.
New or first-time users should make themselves familiar with the specifics of SALT as a telescope (Sec 2 on how SALT differs from other telescopes of its class and what its limitations are, and Sec. 4 on SALT’s characteristics and performance), and the details of how to write the proposal (Sec. 3). Section 1.2 gives useful tips on how to make best use of the telescope and its instruments and how to increase the likelihood to get time allocated and the observations executed. Both the section on how calibrations are done or requested (Sec. 5) and how to calculate overheads (Sec. 10) are important on calculating the overall time request. Every instrument section presents first an overview of the status of that instrument (what is available in this semester, what to look out for and possible caveats), followed by detailed descriptions on available modes, filters etc including descriptions on performance. Important is also the last subsection with the information on what kind of calibration observations are offered for free and which calibrations the user can choose for themselves. A glossary on SALT-specific expressions and acronyms can be found in the appendix as well as details on technical information on the instruments.
SALT is an optical 10-m class segmented-mirror telescope situated at a dark site in Sutherland, South Africa. SALT is especially suited for spectroscopic and high-time resolution observations. SALT is fully queue scheduled with possibilities for real-time input from the PIs and fast turnaround data delivery. Target visibility is in the range of DEC = +11 to –76 deg.
Figure 1.1 shows a smoothed “heat-map” of the number of Observing Blocks (Sec. 2.6) visits over four semesters in 2015 and 2016. The distribution is very non-uniform, areas with a very high number of proposed visits include e.g. the Magellanic Clouds, the Galactic Bulge, some Deep Fields and Equatorial fields. It is thus not possible to execute all of the blocks even if they had the highest priorities. Note however that track times (see Sec. 2.5) are much longer at deep southern declinations, while visibilities are longer at the equator, increasing the likelihood that such targets get observed over those in oversubscribed areas.
Figure 1.1: Smoothed “heat-map” of the number of Observing Block visits over four semesters in 2015 and 2016 (red: highest visits, blue: lowest visits).
Time allocation is done by Priorities (Sec. 3.4). Figure 1.2 shows the average realised completeness of time per priority over the past five semesters. For P0 (time critical observations only) the completeness refers to the triggered observations.
Figure 1.2: Completeness of Observing Blocks by priority, for 2015 – 2017.1
SAMS, an active mirror alignment system with edge sensors, was installed on the primary mirror in April 2016. SALT image quality drastically improved and most notably is stable during the night, making all modes of observations more efficient. RSS optics are cleaned every 18–24 months; the most recent service was performed in August 2016. All instruments and the telescope are close to their nominal expected efficiencies for 2018-1. There is a likely 4-6 week shutdown period scheduled for March/early April 2018 to install a new and more efficient RSS guider, though this does not affect the Phase-1 from the PI perspective.
SALTICAM, RSS, HRS and BVIT will be available in the forthcoming semester, but with the following restrictions. More details can be found later in the document in relevant sections.
The SALT semester definitions are:
Semester 1: 1 May to 31 October (deadline late-January)
Semester 2: 1 November to 30 April (deadline late-July)
The current period, 2018 Semester 1 (i.e. for proposal codes starting with 2018-1), runs from:
1 May 2018 to 31 October 2018.
The call for SALT proposals for 2018-1 opens on:
20 December 2017.
The deadline for Phase 1 proposal submission is:
31 January 2018 at 16:00 UT.
The deadline for Phase 2 proposal submission is:
13 April 2018 at 16:00 UT.
Late Phase 2 submissions, unless discussed with the liaison astronomer before the deadline, will not be activated and will therefore not be observed.
SALT is a fixed altitude telescope and is closely modeled on the Hobby-Eberly Telescope (HET) concept. The design comprises a spherical primary mirror mosaic of 91 identical 1 m wide hexagons, tilted at a constant zenith distance (37 degrees), with azimuthal rotation only for target acquisition, see Fig. 2.1. The target is then tracked by moving the instrument payload at the primary focus (“tracker”, see Fig. 2.2). The payload tracker has a range of +/- 6 degrees. The spherical aberration corrector (SAC) provides an F/4.2 beam with an 8 arcminute field of view at prime focus.
SALT can access ~70% of the sky observable at Sutherland, but only during specific "windows of opportunity" (see Sec. 2.5). Objects are not always accessible by SALT, even though they may be above the horizon. However, the dates an object can be observed during the course of a year are almost identical to that of a more traditional telescope.
Figure 2.1: SALT telescope structure with instrument payload and tracker. The telescope can move only in azimuth while the tracker can only move up and down the structure which supports it.
Figure 2.2: Tracker with instruments (payload); the RSS is visible at the top and the SAC is the grey cylinder underneath.
SALT is operated as a queue-scheduled telescope. There is a dedicated group of 8 SALT Astronomers that observe the targets for each individual program, depending on the current weather conditions and the constraints placed by the PI, in any given night. Each target is assigned a priority, a score that is based on the particular requirements of the proposal, the time that the target is available for the rest of the semester, and other factors. Thus, at any given time during the night there will be a list of targets to choose from, and the SALT Astronomer working at the telescope is responsible for observing the highest scoring and highest priority target that matches the observing conditions to collect the data on behalf of the PI. This queue-scheduled operation of SALT makes use of all available observing time in the most efficient manner.
As part of the SALT design, the pupil (that is, the view of the mirror as the tracker sees it) moves during the track and exposures, thereby constantly changing the effective area of the telescope, see Fig. 2.3. Because of this, accurate absolute photometry and spectrophotometry are not feasible. Photometric calibration of imaging must be done using external data of the same field, though internal colour information can be obtained using filter cycles in the case of short exposures (see https://sciencewiki.salt.ac.za/index.php/File:Salticam-phot-nov2011.pdf for more details). Spectrophotometric standards are routinely taken and can be used for relative spectral (shape) calibration, but not for absolute flux calibration.
Figure 2.3: The pupil (yellow) for three different tracker positions. The grey areas are non-illuminated parts of the mirror.
SALT tracks in two modes: closed loop and open loop. In closed loop the telescope position is controlled automatically by a guidance probe and focus can be adjusted as required. This is the standard mode for spectroscopy. In some cases when doing imaging, guidance may not be available and then open loop tracking is employed. In this case the position and focus may drift slightly and short exposure times are recommended (see, e.g., Sec. 6.9).
The altitude restrictions on SALT (47º to 59º) place observing constraints in terms of instantaneous sky access in Hour Angle and Declination, which is shown in the visibility or so-called SALT “toilet seat” diagram in Fig. 2.1. Prominent astronomical objects are marked at their respective declinations. Only objects inside the annular region are observable by SALT at any given time. Objects at southerly declinations are visible for longer periods (several hours, e.g., the LMC) compared to those at northerly declinations, where the average time for a single track is only 50 minutes. For all except the most northerly or southerly declinations, objects can potentially be observed twice a night at favorable times of the year. The airmass over SALT’s elevation range varies from 1.17 to 1.37 with a mean of 1.25.
Figure 2.1: The visibility annulus of objects observable with SALT, as a function of declination and hour angle. The hashed regions show the range of motion for the tracker at two different declinations.
The total maximum observing time, or visibility, for a celestial target is defined as the time it takes to transit the annulus, which is dependent on the Declination. But while the telescope can access any point within this visibility annulus, the length of time a target can be tracked is not only restricted by the boundaries of this annulus, but also by the tracker movement (see Fig. 2.1) since the telescope structure cannot be moved while observing. Thus the maximum track length for an object, is equal to or shorter than the visibility time. The two hashed regions in Fig. 2.1 are examples of areas that can be reached by moving the tracker alone (that is, without moving the telescope). In other words, it is this maximum track time (and not the visibility) that defines the maximum length of an observing block (see Sec. 2.6). Of course, while the target is still visible, a new pointing can lengthen the total observing time by moving the telescope structure to a new azimuth position and starting a new observation.
For example, Equatorial targets lie in the zone where two visits per night are possible (e.g., the Galactic Centre target in Fig. 2.1), but they have highly constrained track times with, in practice, around 45 mins maximum to use for an exposure (in addition to the pointing/acquisition), see Fig 2.2. The longest track times of more than 2.5 hours can be achieved for very southern targets.
Figure 2.2: The “actual” total maximum track time for objects as a function of Declination.
For planning purposes it is essential that the PIs use the Visibility Calculator (see Sec 3.7), which gives more accurate information than Fig. 2.2.
Figure 2.3 shows a snapshot with the target information to the left and track length information to the right. The total visibility is shown in the lower left under `source availability’, in this case 15827 seconds (note that for targets at intermediate declination there will be two entries, one for each visibility area in the annulus). The track times for a give starting time in the night can be seen by clicking at any location of the visibility curve, e.g., 3529 seconds for the position shown in the plot.
Note that it is not recommended to use track lengths much longer than one hour because weather conditions may change rapidly. Any Observing Block longer than one hour will be accepted by the observer after this time, even if the conditions deteriorate (see Sec 2.6 for more details). In addition, the dynamic scheduling makes it difficult to choose the exact starting time of an observation, so if a track length is too close to filling the whole visibility window it may be difficult for the target to be observed at all (see Sec 2.6 for more details).
Note that if the target list is long, the PIPT gives the option to create a visibility table using the menu item Target > Create Multitarget Visibility Table which will help to calculate all the visibilities.
Figure 2.3. The SALT Visibility Calculator includes a tab displaying the available track length (the red curve) for a target.
All SALT observations are executed using Observing Blocks. These are defined as the minimum schedulable unit. A block must be allocated a single priority and have a single Moon brightness, seeing range, and transparency specification.
A block will consist of:
This sequence of observations in the block plus all necessary overheads must fit within the target’s maximum available track time, inclusive of canonical overheads (900 seconds for MOS, 1500 seconds for BVIT, 500 seconds for HRS and 600 seconds for any other instrument mode). It is thus useful to economise on the number of blocks to increase observing efficiency – but note the caveats below. Be aware that a target’s track time is less than or equal to its visibility time (Sec. 2.5). For a discussion on the ‘Too Tight Track’ (TTT) syndrome (where there is only a very short time window within which the SALT Astronomer can point to the target to obtain the track length required) please check our website: http://astronomers.salt.ac.za/tips-and-tricks/.
A block will be executed under the specified weather conditions. If the weather conditions change within the hour, the block will be rejected and placed back in the queue for further attempts. If more than an hour has already been spent on a block, it will be accepted regardless (which argues for shorter block lengths and repeated blocks to reach the required exposure time).
A block will also be rejected and placed back in the queue if the data quality was compromised by technical difficulties with the telescope or instrument within the first hour of the block. (Note that the data will still be available to the user).
Note that acquisition images are provided solely as a means of field identification and to allow positioning of the target(s). Acquisitions may thus be out of focus or otherwise unpalatable-looking: track time is valuable, and we do not want to waste time tweaking the acquisition images. The image quality will be refined before science data are taken. If focused SALTICAM images are required for science reasons, please add the relevant instrument configuration to the block. For RSS longslit observations, at least one in-focus SALTICAM slitview image will be provided.
Observing Blocks will be created in detail in Phase 2, but it is necessary to be aware of the basic principles when planning observations for Phase 1.
Since SALT is a service mode telescope, the SALT proposal cycle consists of two phases: Phase 1 is the request for observing time and, after approval by the Time Allocation Committees (TACs), Phase 2 is the preparation of the approved observations.
The scientific justification of the program is the crux of Phase 1 and is evaluated by the relevant TAC, while SALT Astro Ops reviews the technical justification. Target information (where known), including numbers and lengths of visits to targets, is required already at the Phase 1 stage, as well as a high-level selection of an observing mode. The final detailed observing configurations of programs accepted by the TACs will then be submitted as part of Phase 2, and will be reviewed by the Astro Ops prior to being added to the observing queue. Changes to the target lists and other observation details may still be made at this stage within the constraints of the science goals in the proposal accepted by the TAC.
All proposals are created and submitted with the proposal and observation preparation tool (PIPT; see Sec 3.7 for details), both for Phase 1 and 2. Phase 1 proposals may be submitted, edited, and re-submitted at any time before the deadline, as many times as needed. After the deadline, edits are no longer possible. Late submission policy is given in Sec 3.2.
Any questions during the submission phase should be emailed to firstname.lastname@example.org. With the first submission of a proposal it will have been assigned a program code – in that case, that code must be provided in the subject line. See Sec. 3.7 for further details.
Items that need to be entered for the Phase 1 proposal include:
Once the TACs have approved proposals and allocated time according to priority class (see Sec 3.4), the Phase 2 proposals have to be completed adhering to these allocations (Sec 3.9). ToO alerts can be triggered any time during the semester (Sec 3.9.1). Data can be retrieved either as raw data files or pipeline-reduced files (Sec 3.10). All PIs and Co-Is are invited to note our Publication and Acknowledgment Policy in Sec 3.11.
Normal SALT proposals can only be submitted by astronomers who are members of a SALT consortium institution (Sec A.2), or are collaborating with such astronomers. Time can be requested from different SALT partner TACs according to the nature of the collaboration and it is entirely up to the PI and Co-Is to decide what fractions are requested from each TAC.
DDT proposals, on the other hand, can be submitted by any astronomer and no time will be charged to any SALT partner.
At the present time observing time is charged (that is, counted against the allocated time) on the basis of completion of requested observing blocks as they appear in the PIPT and SALT Web Manager.
Guidelines for the TAC regarding late submissions:
Late submissions that show no evidence of an attempt to submit or to make contact with Astro Ops before the deadline should be rejected, though the TAC may decide to accept the proposal following consideration of an appeal from the PI.
In any case, acceptance or rejection should be decided by the TAC(s) and communicated to SALT Astro Ops within 3 working days following the original deadline, after which no further proposals will be added to the database.
There are five proposal types which can be selected in the PIPT only when a new proposal is opened:
Only the first two proposal types (SCI, MLT and LSP) require a Phase 1 submission, but the details required depend on the type.
If there are co-investigators from multiple partners in a single proposal, it is up to the Co-Is to divide the proposed time between the relevant partners, or request all of it from one partner. If a program applies for time from more than one partner, all the relevant TACs will receive the application and will allocate their time individually. It should be noted, however, that some TACs may look with disfavour on proposals from other partner institutions which request the majority of time from them if the respective Co-Is are minor players in the collaboration.
Science proposals come in two flavours:
Regular science proposals can request up to 150 hours and require a single semester to finish.
If you need to continue your program in the next semester, you may either submit a new proposal or submit a proposal progress report, as explained in the section on long-term programs (MLT). The functionality to submit a progress report will become available in early January 2018.
Science proposals with up to 150 hours requested but which can or should be carried out over two or more semesters are called long-term programs. They will need to be specified as such in the Phase 1 proposal submission (the PIPT main page provides a box for Add time request for semester XXXX-X) and require a specific multi-semester justification.
These proposals, if approved for the current semester, will be automatically re-submitted for the next. However, a brief progress report is required for the follow-up semester(s) and must be submitted by the usual Phase 1 deadline. A form to enter this progress report is available on the proposal’s page in the Web Manager (https://www.salt.ac.za/wm/).
Please note that the TACs may re-adjust the time allocation before each semester. If no progress report is received, the TACs may decide not to continue the programme. If no time is allocated by the relevant TAC(s) in any given semester the proposal is no longer supported (i.e. the MLT status has been revoked). A new proposal will need to be submitted if more time is needed to complete the scientific goals.
Science proposals requesting more than 150 hours from one or more SALT partner, which can be spread over a total of six semesters, are called Large Science programs. PIs considering submitting such a program should send an email to the head of Astro Ops at email@example.com with their intention to submit at least two weeks prior to the deadline to discuss overall feasibility and strategy.
LSP proposals will need to be specified as such in the Phase 1 proposal submission. The Phase 1 process is the same as for other proposals with the following exceptions:
LSP programs do not have any requirements on how the data are shared or how the time is distributed.
LSPs should only propose for commissioned modes of instruments which are listed in Sec 1.3.2. The proposal should include a strong justification for the total amount of time required. Science goals should be feasible. Programs with stringent conditions, poor target visibilities, or otherwise difficult observations will not be favored currently. However, proposals for any type of science will be considered as long as the proposal is of very high scientific merit.
The criteria on which the LSPs will be judged are more stringent than for normal science proposals:
As with all multi-partner programs, time will be allocated by the individual SALT partners specified in the proposal submission. In case of LSPs, though, Astro Ops will coordinate communication and discussion between the TACs before final allocations are made. Prior to the final allocation, comments from the TAC(s) will be distributed to the PIs of LSPs and the PIs will have a chance to reply or to adjust the proposal accordingly.
As for long-term proposals, approved LSP proposals will be automatically re-submitted for the next. However, a brief progress report is required for the follow-up semester(s) and must be submitted by the usual Phase 1 deadline. A form to enter this progress report is available on the proposal’s page in the Web Manager (https://www.salt.ac.za/wm/). Time and allocations are not guaranteed for future semesters, but require satisfactory progress being made on the proposals. TAC(s) may adjust their allocations according to how the proposal is progressing.
A Phase 2 proposal needs to be submitted for Director’s Discretionary Time (DDT) proposals (that is, Phase 1 stage is not necessary). These do not need to follow the normal proposal cycle.
A total of 15h per semester of DDT time is available at present (see here for any possible changes or news). This time is not part of the SALT consortium time and thus DDT proposals can also be submitted by any astronomer including those that are not member of one of the SALT consortium institutions (or collaborating with a member).
DDT programs must abide by the following rules:
Commissioning proposals are usually only submitted by members of the relevant instrument team and the SAs. Please contact firstname.lastname@example.org if more information is required.
Science Verification proposals are only available if a special Call for Science Verification proposals goes out once a new instrument or mode has become available and has been commissioned by the instrument team. This call will not follow the usual semester deadlines. The Call for SV proposal document will contain all necessary information.
An individual observing program will consist of a number of Observing Blocks (Sec 2.6) of different targets which will be assigned a set of priorities by the relevant TAC(s). The priorities just influence the likelihood of a given target being observed on a particular night and over a semester, see the Fig. 1.2 in Sec 1.2.
For the upcoming semester, the available science time will be allocated to the different priorities such that 40% for P0+P1 time, 40% for P2 time, and 20% for P3 time with a factor 3 over-subscription rate for P3. These are applicable to both the regular science as well as the large science programs. The percentages are the same for each TAC and all observations are charged in the same manner (see Sec. 3.1).
Highest rated Targets of Opportunity (ToO) programs or time critical observations only. Once scheduled, and weather permitting, Priority 0 observations will have the highest chance of being observed at the time requested. Examples of such observations might include supernovae and other transient events, and rare periodic phenomena.
Any proposal can include time critical observations, but only those allocated a P0 priority will in general be observed in preference to other priority classes.
Note that P0 time is not permitted for non-time critical targets, P1 will be used instead.
Highest rated proposals or observing blocks, which, if scheduled, will have a high chance of being observed in a given night. Such targets will be the most scientifically compelling of all standard (i.e., P1 – P3) priority targets and completion of most P1 blocks in a given semester is expected. We expect to achieve at least 80% completion of P1 blocks, with the main problem being conflicting target distributions.
P2 programs or observing blocks are not as highly rated as P1 by the TACs, but are still considered to be compelling. P2 blocks will have a good chance (60%) of being completed in a given semester.
P3 programs or observing blocks are lowest priority science as assigned by the TACs, but still worthy of consideration. P3 proposals are deliberately over-subscribed by a factor of 3 in order to always have a full queue. If P3 blocks and programs are intelligently designed, that is, to be easy (short, loose constraints, wide RA-ranges with optional targets), dynamic scheduling will likely mean that more than the expected 20% will get observed.
This is a special priority class consisting of “filler” targets, to be done in marginal observing conditions (i.e. poor transparency or bad seeing) or to fill gaps in the observing queue. They would not need to be strictly 10-m class science, but deemed to be useful science nevertheless. P4 programs will not be charged. Contrary to the other priorities, P4 priorities are identified by the PI who should justify in the application (technical section) why their proposed programs should be considered P4 time (e.g. brightness, observing mode, allowable conditions, large pool of short observations). The TAC(s) will accept or reject the P4 proposals as they see fit. P4 programs will only be attempted if, at the duty SA’s discretion, there are no other viable P0 – P3 programs that can be attempted. Please note that P4 programs should ideally consist of short observing blocks, so that they may be slotted in as needed. As with the P3 programs, that is, if designed well, experience has shown that P4 programs can in fact get high completion fractions.
Note that SALT Operations allows any TAC accepted program to add P4 blocks to their Phase 2 program free of charge, over and above their TAC time allocation – contact email@example.com if interested to do so.
There are two types of SALT targets:
We stress that the use of optional targets, especially when they have a wide RA-range, is extremely effective. You can significantly boost the chances of getting your program done if there is always one of your targets visible in the queue.
The PIPT allows entry of observing constraints for the proposal. While individual constraints per target will only be needed for the Phase 2 proposal, the Phase 1 proposal requires information on the tightest observing constraints regarding seeing and cloud cover.
PIs are free to specify any Lunar illumination fraction between 0% to 100% to define the maximum allowable lunar illumination for each observing block in Phase 1 proposals (under target information). In terms of often-used Dark, Gray, and Bright time terminology:
The PI is free to choose any fraction. For example, for a traditional Dark object the PI would use <15%, but if they were to specify a different fraction, e.g., <25% or <40%, they will get more flexibility in scheduling and thus a higher chance of completion. Note that the Bright targets, e.g. with <70% or <100% (i.e. the traditional Bright targets) will also be in the queue when Moon is darker. PIs with equatorial targets please note that the Moon will likely be too close to the target for roughly ~50% of the traditional Bright time. During actual observations our scheduling tools will promote a dark block over a brighter block in dark time, but observations can be scheduled more efficiently when more blocks are available to choose from.
The PIPT for Phase 1 allows the specification of Lunar illumination for each target. Along with the proposal, the TACs will receive a summary on the approximate fractions of the proposed targets for the various Moon conditions. This information serves as a guideline only. The TACs will not specify a Moon condition for a program, they will only allocate time and priority. However, ideally all TAC partners should attempt to distribute their observing time allocations evenly over the range of Lunar phases.
In Phase 2, there will be an opportunity in the PIPT to select also a minimum angular Lunar distance; note that a default minimum angular Lunar distance of 30 degrees is already given, which of course can be changed if necessary.
PIs should also use the instrument simulators (Sec. 1.6) to ensure that overly demanding observing conditions are not requested unnecessarily.
The standard measure of atmospheric turbulence is the Fried parameter, r0. The SAAO (Sutherland) site uses an automated Differential Image Motion Monitor (DIMM) to measure this routinely and continuously. The blurring of an image at the focal plane of a large telescope, what we refer to as “seeing”, is derived from r0 using the standard model of atmospheric turbulence. It is a function of wavelength (λ) and airmass and the DIMM reports seeing using the convention of λ = 500 nm (essentially V-band) and airmass = 1.0. This is the value that is used to define observing conditions and make scheduling decisions.
Median zenithal V-band seeing, measured from the Sutherland DIMM at ground level, is 1.5” (from measurements made over 2011–2016, see Table 3.1). Since the SALT visibility strip lies between 1.16 and 1.37 airmass this leads in principle to a factor of 1.1 to 1.2 degradation of seeing on average. This is broadly the case as can be seen in the actual distribution of seeing values shown in Fig. 3.1 for the second half of 2016, where DIMM values are compared with data taken by the SALT guider. Note that the the active mirror alignment system (SAMS) was already installed for this period. This means that the actual SALT image quality (IQ) as measured by the instrument guiders is quite close to the zenithal seeing value, which is a drastic improvement from times before SAMS, that seasoned users of SALT should be aware of. PIs should note, however, that we have been experiencing better IQ since the arrival of SAMS, we have not been able to match external seeing below 1.4” since ~June 2017 - the reasons for this are, at the time of this call, being investigated and addressed.
Table 3.1: Median zenithal seeing at Sutherland for past semesters
Median zenithal seeing
Figure 3.1: Seeing histograms from the SAAO DIMM and the SALT guider. The data are taken from the same period of time in 2016 since the SAMS was installed. Note that the guider data are not corrected for the average airmass of SALT observations during this period, so the guider data are actually better than the DIMM (which is closer to the ground). The PIs select their seeing restriction based on the intrinsic Zenith value and they now should expect a similar image quality delivered on the detector, except (at the time of this call) where the external seeing is <1.4”. The reasons for this are currently being investigated and addressed.
Table 3.2: Probabilities for a given seeing or better at the Sutherland site
Table 3.3: Expected image quality performance of SALT in depending on seeing
DIMM zenith seeing
Seeing at average telescope airmass
As an aid to choose the most useful observing constraints, Table 3.2 shows the probability of having a given (or better) seeing, based on all the available seeing statistics. Table 3.3 indicates the expected image quality performance of SALT (in terms of the FWHM and enclosed energy diameters (50% and 80%) of the PSF for different DIMM seeing values (all V-band). The PSF is basically described by a modified Moffat function. The proposers should realise that it is the DIMM zenith seeing number that has to be inserted as “seeing” into the instrument simulator and used as the requested seeing, while the other numbers should be used to plan actual SNR. The simulators automatically correct the inserted seeing at zenith for airmass.
The results of a study looking into the causes of atmospheric turbulence above the Sutherland observing site are presented in Catala et al. 2013.
The cloud cover conditions are
We define thin cloud to range between either occasional thin clouds passing over (e.g. partly clear) to consistent all sky thin cirrus. Thick cloud corresponds to a moderate to heavy extinction and when guidance is often interrupted due to the guide stars being partially or fully obscured for a good portion of the track. Short exposures of bright stars are best suited to thick cloud conditions.
All investigators (PI and Co-Is) on a SALT proposal must have an account on the SALT server before the proposal can be submitted. This can be created by means of the Web Manager by pointing a browser to https://www.salt.ac.za/wm/Register/. After a successful registration, a confirmation email is sent, which includes instructions for validating the chosen email address.
Once an account has been created, the Web Manager can be used to view one's proposals (including unsubmitted ones) and to update one's contact details.
All proposals are created and submitted with the proposal and observation preparation tool (PIPT), both for Phase 1 and 2. This is a stand-alone application requiring Java 1.8 or higher. While the Open JDK may work, using the Java environment provided by Oracle is strongly recommended. (http://www.oracle.com/technetwork/java/index.html). The PIPT itself can be downloaded from http://astronomers.salt.ac.za/software/. A manual for the PIPT is available both as html and pdf.
The scientific and technical justification needs to be generated from a Word/Latex template, which can be downloaded from
Some common questions and issues are addressed below; however, a more complete, live, and frequently updated online FAQ is available at:
In the PIPT, new proposals can be created with the File > New Proposal menu item. The PIPT will ask which type of proposal to create (see Sec. 3.1). Note that only a Science or Large Science proposal will be forwarded to the TAC (see Sec. 3.3 for details).
The main items to be entered in the PIPT for Phase 1 are:
All but the last two bullet points are entered in the respective boxes in the PIPT form, while the last two items must be included in the form as a PDF. This PDF file is limited to four pages in length (eight pages for Large Science Proposals). The PDF must be generated using the latest version of one of the templates provided (in Word, OpenOffice, or LaTeX format). These can be downloaded from http://astronomers.salt.ac.za/proposals/proposal-templates/. Note that Large Science Proposals use a different template from the rest of the proposal types. You have to use the template for the current semester; you cannot reuse templates from the previous semesters. Word limits quoted in the template should be considered guidelines as long as the total proposal length is less than four (eight) pages including references and figures.
SALT observing programs distinguish between the Principal Investigator (PI) and a Principal Contact (PC). The later will be the actual liaison between the proposing team and the SALT team, do the Phase 2 proposal preparation and submission, receive the data etc. For large collaborations it may be desirable to set up a group emailing address so that several people can share in. Note that only the PC will receive communication through the Web Manager regarding clarifications on the proposal, questions and information during observing and notifications when the data becomes available.
Targets and instrument configurations have to be defined for a Phase 1 proposal. These may be added by right-clicking on a node in the navigation tree (on the left). Similarly, adding and removing content from a table can be accomplished by right-clicking on the table.
Warnings should be taken very seriously, as they often indicate a serious flaw in the proposal. In most cases, submission is only possible once the problem has been fixed. An explanation is displayed by clicking on the little warning sign next to the problematic input.
Before a proposal is submitted, it should be validated with the menu item Proposal > Validate. If the validation fails, this usually means that some required input is missing. Note that valid Phase 1 proposals may be submitted, edited, and re-submitted at any time before the deadline, as many times as needed. It is recommended to re-submit frequently to ensure that the final submission goes smoothly and does not cause unnecessary delays in the final submission.
After the first successful submission of a proposal, a confirmation email with the proposal code is sent to all investigators. This proposal code uniquely identifies the proposal, and it should be quoted in the subject line of any email query related to the proposal. The proposal code is also added to the proposal itself, so that resubmissions do not generate new proposals in the database. It is a good idea to double-check that the correct proposal code is shown in a submitted proposal. Confirmation emails for re-submissions are only sent to the investigator re-submitting the proposal.
When logging in to the Web Manager, a list of the user's proposals is shown. Clicking on any of the proposals leads to a page with the proposal details, which may be used to check a submitted or re-submitted proposal. However, it may take a few minutes before the content is fully visible after submission (especially finding charts). It is also possible to import a proposal in the PIPT (using at the top menu bar: either File -> Import from Zip file or Online -> Import from Server), e.g., for a Co-I to access a current proposal, or to recover an old proposal. Note that when a proposal of the same code already exists on the user’s computer, the version on the computer will be replaced with the imported one (the user will be warned beforehand).
In addition to the the Web Manager and the PIPT, a Visibility Calculator and Simulator Tools are supplied for SALTICAM, RSS and HRS, which can be used to plan the required instrument setup and the necessary exposure time (see Sec 1.6 for all downloads). They also require Java 1.8. These Simulators allow the user to define a target spectrum and an instrument configuration, and to calculate the signal-to-noise ratio expected for these. They are always updated to the latest information regarding sensitivity, throughput and other instrumental constraints so please make sure you have the latest version. It should be noted that the Simulators do not take any overheads into account when calculating the signal-to-noise ratio.
The PIs should be aware that the wavelength ranges predicted by the RSS Simulator currently may have inaccuracies up to +/– 2 nm.
Simulated setups can be saved from the Simulator Tools, and these saved setups should be attached to a Phase 1 proposal in the PIPT for use in the technical reviews (under the Instrument Configuration nodes). The technical justification may refer to these attached instrument setups.
All Phase 1 proposals will first be directed to the SALT Astronomy Operations team for a technical feasibility assessment. Comments on technical feasibility will be forwarded to the individual TACs of the SALT consortium. The TACs will then allocate time to successful proposals in various priority classes. The minimum time allocation for a successful proposal will be 900 seconds per priority.
In cases where only a small fraction of the time requested for a multi-partner proposal is awarded by the relevant TACs, the SALT Astronomy Operations Manager will engage with the relevant TAC Chairs to ensure that the allocation can actually result in a meaningful program.
After the full TAC review and time allocation process has been completed for all partners, PIs will be notified of the outcome. These notifications mark the start of the Phase 2 submission period.
The notifications of the TAC outcome mark the start of the Phase 2 submission period, during which the detailed observing blocks must be submitted by the PCs to SALT operations using the PIPT. Changes to the target lists and other observation details may still be made during this stage within the constraints of the science approved by the TAC. Any other changes need the approval of the Head of Astronomy Operations who may refer the request to the relevant TACs.
Proposals with Phase 2 material submitted early may be considered for observations even before the new semester observations officially commence, depending on the status of the queue of the previous semester projects. There is a strict deadline for the Phase 2 submission phase (see Sec. 1.5), which is crucial for planning the schedule for the semester. We cannot guarantee that programs submitted after the Phase 2 deadline will be included in the observing queue. If there are problems causing delays please be in contact with SALT Operations before the deadline.
For a Phase 2 proposal, the PIPT will ensure that:
ToO programs that do not yet have targets available should submit dummy block(s) so their configurations can be reviewed. For normal proposals, all targets must be submitted at the deadline, but updates (within the constraints of the approved science) may be supplied throughout the semester if required.
All accepted SALT proposals will be assigned a Liaison SALT Astronomer (LSA) who will be the main point of contact between the PI and SALT Ast Ops. Communications regarding the completion of the Phase 2 proposal, the status of the proposal and issues regarding the observations and data should be communicated with the LSA in the first instance. Do not forget to quote the proposal ID in the subject line of any email communication.
For activation of ToO programs, PIs or PCs should communicate their request to firstname.lastname@example.org. For short notice or urgent real-time alerts, the SALT control room telephone number (+27 23 5711356) can be used to contact the duty SA directly.
The PC of the proposal will receive an email with download instructions as soon as the data are ready to be downloaded, generally the morning after the data have been taken. This includes the raw data, processed data (see Sec. 3.10.2), and documentation including the night log. Due to disk space constraints, the data will remain on our ftp server only for two weeks. However, the PC may request a dataset again. Please visit the Web Manager and load the relevant proposal. The data can be requested in the last column from the table listing the observations taken for the proposal. The relevant data will then be placed in the public ftp server for another two weeks, and the PC will be notified by automated email when the data are ready to be retrieved. This should happen fairly quickly, so please contact us at email@example.com if you do not receive the email notification within 24 hours.
Standard star calibrations taken with the same setting as the proposal may also be requested using the Web Manager from a button located the bottom of the table listing all the observations taken for the proposal.
The PI has two options for data distributions: Normal and Fast:
A searchable data archive is as yet not available. Please contact the SALT Astronomers for any requests for Commissioning/Science Verification or non-proprietary data.
The proprietary period of the data will be decided by each individual partner. At this time, none of the partners have yet specified a proprietary period. The PI may specify any proprietary period for their data – we suggest an 18-month proprietary period.
The SALT data reduction pipeline processes the previous night’s data at 10:30 am each day. The pipeline will pre-process the data, reduce observations from each of the different instruments, assess the data quality of the observations, and distribute the observations to the investigators.
The pipeline reductions will process all observations for basic CCD reductions. This includes bias subtraction, gain correction, cross-talk correction, and mosaicking the different CCD chips. For HRS data, the pipeline will also wavelength calibrate and extract the spectra.
All of the raw and reduced data will be made available in the SALT FTP directory for the user. This is accessible at ftp://saltdata.salt.ac.za using the users login for the Web Manager as a bzipped tarball file. In addition to the raw and reduced data, the astronomers log, environmental information, and other documentation is also provided in the directory.
The PySALT user package is the primary reduction and analysis software package for the SALT telescope. It is both used in the data reduction pipeline and is available to the user for their own data reduction. It can be downloaded from http://astronomers.salt.ac.za/software/. Currently, these tools include basic data reductions for RSS and SALTICAM in both imaging, spectroscopic, and slot modes. Basic analysis software for slot mode data is also provided. These tools are primarily written in python/PyRAF with some additional IRAF code.
Documentation is available on the http://sciencewiki.salt.ac.za/index.php/PySALT, in user manuals, and also provided within the package itself. PySALT Data Tutorials can be found on the SALT sciencewiki pages at https://sciencewiki.salt.ac.za/index.php/PySALT_Data_Tutorials. A script for fully reducing long slit data is also available here: https://github.com/crawfordsm/zsalt .
SALT RSS data has also been reduced using the IRAF reduction package. A recipe on how to reduce longslit spectra can be found on the sciencewiki at https://sciencewiki.salt.ac.za/index.php/Long_Slit_Reduction_Recipe. A more comprehensive report can be found in http://www.saao.ac.za/~akniazev/pub/SALT_Long_slit.pdf. Furthermore, a recipe on using a combination of packages IRAF, PyRAF and other packages can be found in http://www.saao.ac.za/~akniazev/pub/RAIL_README.pdf.
Analysis software for RSS spectro-polarimetry is available at https://github.com/saltastro/polsalt.
Please notify firstname.lastname@example.org of any publication made using SALT data including reviewed papers and conference proceedings.
All science papers that include SALT data which are submitted for publication in refereed science journals must include the following words of acknowledgment:
“All/some [choose which is appropriate] of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under program(s) [insert Proposal Code(s)].”
We recommend that the Principle Investigator is also mentioned after the Proposal Code. In addition, for papers which predominantly based on SALT data, a footnote symbol should appear after the paper title*, and the following text should be written as a footnote:
*based on observations made with the Southern African Large Telescope (SALT)
If possible, please also include the Proposal Code and Principle Investigator in body of the paper when describing observations.
If you use data reduced by the SALT science pipeline or use the PySALT software, please provide a link to http://pysalt.salt.ac.za/ and cite the following paper:
Crawford, S.M., Still, M., Schellart, P., Balona, L., Buckley, D.A.H., Gulbis, A.A.S., Kniazev, A., Kotze, M., Loaring, N., Nordsieck, K.H., Pickering, T.E., Potter, S., Romero Colmenero, E., Vaisanen, P., Williams, T., Zietsman, E., 2010. PySALT: the SALT Science Pipeline. SPIE Astronomical Instrumentation, 7737-82
In addition, the following papers provide a description of the telescope and instruments:
Buckley, D.A.H., Swart, G.P., & Meiring, J.G. 2006, Proc. SPIE 6267, 62670Z
Burgh, E. B., Nordsieck, K. H., Kobulnicky, H. A., et al. 2003, Proc. SPIE, 4841, 1463
Kobulnicky, H. A., Nordsieck, K. H., Burgh, E. B., et al. 2003, Proc. SPIE, 4841, 1634
Rangwala, N., Williams, T. B., Pietraszewski, C., & Joseph, C.L. 2008, AJ, 135, 1825
O'Donoghue, D. et al. 2006, MNRAS, 372, 151
Barnes, S.I., et al 2008, Proc. SPIE 7014, 70140K
Bramall, D.G., et al 2010, Proc. SPIE 7735, 77354F
Bramall, D.G., et al 2012, Proc. SPIE 8446, 84460A
Welsh, B., D. Anderson, J. McPhate, J. Vallerga, O. Siegmund, D. Buckley, A. Gulbis, M. Kotze, and S. Potter, High Time-Resolution Astronomy on the 10-m SALT, New Horizons in Time-Domain Astronomy, Proceedings of the International Astronomical Union, IAU Symposium 285, p. 99-102, 2012.
McPhate, J., O. Siegmund, B. Welsh, J. Vallerga, D. Buckley, A.A.S. Gulbis, J. Brink, and D. Rogers, BVIT: A visible imaging, photon counting instrument on the Southern African Large Telescope for high time resolution astronomy, Proceedings of the 2nd International conference of Technology and Instrumentation in Particle Physics, Physics Procedia 37, pp.1453-1460, 2012 (Chicago, 9-14 June 2011)
Section 2 explained the basic concepts to understand when planning observations with a telescope like SALT, especially regarding the track times, the visibility of objects and the effect of the moving pupil for absolute (spectro)photometry. This section will define the characteristics and performance of the telescope and general, instrument-independent issues.
SALT is situated at the South African Astronomical Observatory (SAAO) field station near the small town of Sutherland, in the Northern Cape province, about 400 km from Cape Town. Its coordinates are: Latitude: -32 22 46, Longitude: 20 48 38.5 E, and elevation: 1798 m.
The SALT mirror comprises 91 hexagonal segments figured to have spherical surfaces with a radius of curvature of 26.165 m. When all segments are pointing to a common focus, they act as a 10-m spherical mirror. The effective area for a given observation, however, is more likely that of a 7─9-m telescope for two reasons: (i) only a sub-section of the full mirror is seen by the tracker (the `pupil’, see Sec. 2.3 for more details), and (b) since the instruments are placed in the prime focus, some of the light is blocked by the payload. Both effects vary with the tracker position and thus during an observation. See Sec. 4.4 for details.
Active control of the mirror segments with new mirror edge sensors, called SALT Array Management System (SAMS), has become operational in early 2016 with very encouraging results (see Sec. A.3). Images are now stable throughout the night over large temperature gradients, and observations are only limited by intrinsic seeing and dome seeing. This is a significant improvement from times before SAMS, which the re-current PIs will appreciate. During 2016 it was feasible to request 1.2 ─ 1.5” seeing for faint and challenging targets; good results for e.g. high-redshift point source spectroscopy have already been demonstrated. However, since about June 2017 we have been unable to match external seeing < 1.4” - this is currently being investigated. Also please note that, likely due to dome-seeing issues, sub-arcsec conditions (rare in any case) are still unrealistic to fully take advantage of.
There is strong vignetting of the 8’ x 8’ Field-of-View, as shown in Fig. 4.1. Objects observed more than 2 arcmin from the centre of the field receive up to 10% less light (depending on the instrument used), and this needs to be taken into account when planning to make use of targets over the full field of view (that is, this is not incorporated into the simulators). These numbers are greater than the specification and are still under investigation.
Figure 4.1: Vignetting of the FOV with RSS and SALTICAM.
The primary mirror is kept clean by regular (every week or two) cleaning with high-pressure CO2, and individual segments are normally taken out for washing and re-coating in a cycle of nominally about 12 months. This has been standard practice since 2012. Throughput of the telescope is routinely monitored using SALTICAM (since there are no significant optics in this instrument, these values can be thought of as an approximation of the telescope throughput) by measuring standard stars with the primary mirror in “burst mode” where each segment forms an independent image of the star. The left-hand panel in Fig. 4.2 shows the yearly measurements, corrected for the estimated total efficiency of the instrument (filters, CCD, foreoptics) and the atmosphere. Only the 7–10 best quality mirror segments were used to derive these numbers, while the values implemented in the Simulator are taken to be 15–20% worse to describe a typical track across mirror segments that are in different stages of cleanliness. The Simulator values are kept up-to-date.
For comparison, the nominal expected curve as well as the system specification are shown as well (in light blue). The effect of not cleaning the primary regularly is illustrated by the historical 2006–2008 throughput values of the mirror which dropped significantly with time. The values for 2012 – 2014 (black curve) are an average. In June 2015 the Atmospheric Diffraction Corrector (ADC) was cleaned (see red curve), and in August 2016 the Spherical Aberration Corrector (SAC) partially cleaned (see dark blue curve). The currently measured telescope throughput numbers are shown as the dark blue points. We are closer to the expected throughput in the red part of the spectrum than we are at blue and intermediate wavelengths. We suspect an aging SAC is the largest contributor to the slightly less than optimal system throughput, but a full recoating is not likely for a while.
Figure 4.2: Left: Current and historical telescope (that is, SALTICAM) throughput values for different wavelengths (in micrometer) are compared to expectations. The most recent values are shown in dark blue. Measurements correspond to the 7–10 best quality mirror segments. Right: RSS optics throughput values. The dashed line was derived by Ken Nordsieck in 2013 and has been adjusted by the factor of approximately 1.6 improvement in efficiency due to the 2014 RSS intervention and 2015 ADC clean. The blue points show mean values from measured on-sky photometry in 2015, 2016, and 2017, when they have stayed quite stable.
The RSS instrument-specific throughput had been significantly reduced over all wavelengths since the re-commissioning of the instrument in 2011. A major overhaul of RSS took place in September and October of 2014 during which many of the optics were cleaned and optical coupling fluids in the collimator were replaced. This resulted in approximately 40% increase in RSS throughput (and more in the blue part of the spectrum) judged from both pre-installation laser measurements and on-sky standard star measurements. Additional causes of poor throughput were attributed to several degraded coatings though the fixing of these is now on-hold due to lack of funding. A new optical service was done in August 2016 which recovered the slowly deteriorating RSS efficiency (by about 10%) to the clean 2014 values. The 2017 values are also similar. It is now planned that RSS will undergo a routine optics clean every 24 months or so.
The dashed line in the right panel in Fig. 4.2 shows the RSS throughput derived from a large number of spectrophotometric standard stars by Ken Nordsieck in June 2013, now multiplied by a factor of 1.6 to approximate the current situation. A direct absolute RSS measurement using “burst mode” in 2015 is shown as the blue points. Note that the efficiency of RSS observations is naturally also affected by the telescope throughput.
We stress that the current throughput values as discussed above are incorporated into the latest instrument Simulators which should be used for planning of 2018-1 programs. Any noticeable changes will be immediately incorporated into the simulators, and, where necessary, the community will be informed. Finally, note that while the atmosphere is corrected out from Fig. 4.2, its effect is included in the Simulator tools and can be adjusted therein.
The nominal collecting area of the primary mirror with a central track after all obscurations are subtracted, is ~55 m2, decreasing to ~40 m2 for extreme off-axis tracker positions. This means that SALT is equivalent to between a ~7 to 9 m diameter conventional telescope depending on the pupil (Sec 2.3).
The current default collecting area in the instrument Simulators is set to 46 m2 (or approximately 53 fully illuminated segments) – this corresponds to experimentally derived averages of visible pupil area with tracker obscuration over a full track, and also makes allowance for the fact that the throughput calculations referred to above are normally done for a dozen or so best-quality segments. The collecting area is an adjustable parameter in the Simulators, but it should only be changed with caution.
SALT calibration data are divided into four categories:
Please see the instrument-specific sections for the current semester calibration plans. No calibrations are needed for BVIT.
SALTICAM is available for the 2018-1 semester. There is a new website that lists the installed SALTICAM filters live and should be used for the Phase 2 proposal preparations: http://astronomers.salt.ac.za/status/.
Though guiding with SALTICAM is possible, it has several features rendering it not that useful for many applications (see Sec. 6.9). Overall, we suggest limiting SALTICAM exposure times to approximately 120 seconds with open-loop tracking, or single filter observations utilizing a bright guide star (usually chosen by the SA; PIs can indicate preferred choices on charts though they may not always be accessible).
SALTICAM is a UV–Visible imaging and acquisition camera, capable of high time resolution imaging (down to 0.05 seconds). It consists of two E2V 44–82 CCDs (2048 x 4102 x 15 µm pixels), which are physically separated by a 1.5 mm gap and are read out by four amplifiers. SALTICAM is at prime focus; however, it is fed by a fold mirror and has a reduced focal ratio of f/2. The result is a nearly 10-arcmin diameter field of view, with the central 8-arcmin diameter portion being used for science and the outer annulus for guide stars as shown in Fig. 6.1 (but see Sec. 4.2 on vignetting). The plate scale is 0.138 arcseconds per unbinned pixel. A wide range of filters are available, spanning the wavelength range 320 – 950 nm. Due to the variable pupil, the photometric accuracy is limited to at best 0.05 mag which can be reached for stellar objects using dithering (see Sec 6.9).
More details on this instrument can be found at in the appendix (Sec A.5). A simulator that uses target characteristics and a detector configuration to return count rates, signal-to-noise ratios, pixel saturation, and readout times can be downloaded from http://astronomers.salt.ac.za/software/ .
Figure 6.1: SALTICAM full layout. For details see Sec. A.5.
There are four possible combinations for readout speed and gain settings, returning gain values between 1.0 and 4.5 electrons/ADU with readout noise of either 3.3 or 5 electrons per pixel (Tables 6.1 and 6.2, respectively). The dark current is typically less than 1 electron per pixel per hour. Full well depth is on the order of 170k electrons. Pixel pre-binning from 1x1 to 9x9 (independent in each direction) and up to ten subframe windows can be selected. The readout times for full frame with 2x2 binning are given in Table 6.2.
Table 6.1: Gains for the four different readout modes selectable on SALTICAM
Table 6.2: Readout (RO) times of SALTICAM for the 2x2 binning. Refer to Sec A.5 (`Observer specifics’) for times of other binnings. *Inclusive of CCD readout, disk writes, and software overheads.
Standard modes of operation are normal imaging (full-frame readout), frame transfer (half-frame readout), and slot mode (144-row readout). Specific characteristics for these modes, as well as the specialised modes of non-sidereal tracking and drift scanning, are discussed below. Note that absolute photometry is not possible with SALTICAM alone because of the moving pupil (see Sec 6.6). All the sub-framing, preamplifier binning, gain, and filter options listed for SALTICAM are available in all instrument modes.
Normal imaging is the basic, full-frame SALTICAM mode, which also serves as the acquisition mode for spectroscopic observations.
The frame transfer (FT) mode ensures moderate time resolution (a few seconds) and no dead time. In frame transfer mode, a mask covers the lower half the detector (both chips, see Fig. 6.3, left panel). At the end of each exposure, the image in the top half of the chip is rapidly (0.2 sec) shifted to the lower half where it is read out while the next image in the top half accumulates photons during the next exposure, thereby ensuring no dead time.
A list of the minimum exposure times for frame transfer mode in each binning is provided in the third column of Table 6.3 (note that software reaction times are not included here).
Figure 6.3: SALTICAM schematic for frame transfer (left) and slot mode (right). The gray regions are masked.
Slot Mode (sec)
Frame Transfer (sec)
Table 6.3: Minimum exposure times per binning for SALTICAM Slot Mode and Frame Transfer (FAST readout).
Slot mode ensures high time resolution (down to 0.05 sec) with practically no dead time (~milliseconds). It only works with the FAST readout speed. In this mode, a mask is advanced over the entire detector except for a horizontal slot of 20 arcsec height just above the frame-transfer boundary (see Fig. 6.3, right panel). At the end of each exposure, 144 (unbinned) rows are moved down which allows exposure times as short as 0.05 sec. Timing tests carried out with an independent GPS demonstrate that the absolute and relative timing accuracy of slot mode are good to a few tens of millisec.
The minimum exposure time for slot mode in each binning setting is provided in the second column of Table 6.3 (note that software reaction times are not included here). More information on slot mode is available in Sec A.5.
Please note that the position angle is a critical parameter for most slot mode observations in order to image both the target and a comparison. Finder charts should clearly indicate the position angle and the location of the slot (done automatically by the SALT finder chart tool http://pysalt.salt.ac.za/finder_chart/).
For imaging objects in the solar system, non-sidereal telescope tracking is offered. Initial tests of the implementation and accuracy of this mode at slow (a few arcsec per hour) and fast (hundreds of arcsec per hour) rates have been carried out. The telescope correctly interpolates ephemerides in order to point, but tracking at the correct non-sidereal rates has not yet been commissioned. We have not yet quantified any errors on the pointing. Any non-sidereal tracking proposals are considered shared risk.
Drift scanning is an imaging mode where the telescope is parked at a stationary (central, maximal pupil) position and the CCD readout is clocked at the sidereal rate. This can be used to produce long imaging “strips” on the sky, e.g. for surveys. The mode also side steps difficulties in exact flat-fielding of normal SALT observations which are due to a changing pupil shape.
While some preliminary SALTICAM drift scanning tests have been successfully completed, there are still some issues to iron out before this mode is offered to the community. However, we are interested in starting to gauge interest in the mode so any interested PIs are encouraged to contact email@example.com before proposing, to discuss the needs and details.
SALTICAM has an eight-position filter magazine. Available filters are listed in Table 6.4. The transmission curves can be viewed in the PIPT.
The SALTICAM CCDs were optimised for visible and near UV imaging, thus no effort was made to minimise fringing at near IR wavelengths. We have not yet quantified the amplitude of fringing in all filters. We have observed fringes with an amplitude of ∼10% peak-to-trough for red, narrow-band filters such as z’. Fringing is not an issue for broadband filters or those at the shorter end of the wavelength range.
U, B, V, R, I
u’, g’, r’, i’, z’
u, b, v, y, H-β wide, H-β narrow, SRE1, SRE2, SRE3, SRE4, Clear
H-α (zero redshift)
380-nm (FWHM 40Å)
Table 6.4: SALTICAM filters
NOTE: the text below presents the ideal, expected situation. Flat-fielding in particular remains an unsolved issue, and even relative photometry within the SALTICAM FoV has not been achieved to much better than 5% accuracy (see Sec. 6.10.1 on calibrations for more details).
The moving pupil inherent to the basic operation of SALT presents special problems for doing photometry with SALTICAM. While it is true that if the tracker position is known at all times, the fraction of the primary mirror within the pupil can be calculated (including gaps between mirrors) and the photometric "response" function of the telescope can be worked out. However, this assumes equal reflectivity for all mirrors; clearly this will not be true and furthermore it will be variable as the cycle of mirror recoating runs. (Typically, at least one and possibly two segments per week will be recoated).
Measuring reflectivities of mirrors is an uncertain process so it seems very difficult to provide calibrations sufficient to estimate the response function to at least 1 percent (preferably better) for all tracker positions.
So those carrying out photometry with SALTICAM should bear in mind:
For more information on SALTICAM photometry and flat-fielding, see these two documents (you will need your Web Manager login credentials to access): https://sciencewiki.salt.ac.za/index.php/File:Salticam-phot-nov2011.pdf and https://sciencewiki.salt.ac.za/images_sciencewiki.salt.ac.za/1/1b/SCAM_obs.pdf
All SALTICAM sensitivity calculations for planning observations should be done with the latest version of the SALTICAM Simulator tool (see http://astronomers.salt.ac.za/software/). The tool uses numbers based on throughput tests with the primary mirror in “burst mode” where each segment forms an independent image of the star, as well as Sloan comparison fields, and have been extrapolated for a typical pupil during a track (see Sec 4.3 for details). We have directly verified count rates up to about 5-minute exposures and these behave as expected. Longer integrations are not practical due to the difficulties with auto-guiding (see Sec. 6.9) and SALT’s current open-loop tracking performance.
Thus, the deepest SALTICAM exposures should ideally be constructed from dithered (see below) and co-added short (~2-minute) exposures. For example, recent programs detected targets using co-added 2-minute-frames down to g=24.7 mag and r=24.1 mag. However, whether the ideally scaled signal-to-noise ratio of stacked images is reached depends on e.g. the quality of flat-fields (see Sec. 6.6) and the stability of the PSF of sources over tens of minutes. While the latter has become better with the recent introduction of the active mirror alignment system (SAMS), we nevertheless urge the PIs to be conservative in estimates of deep SALTICAM imaging until proper characterisation has been obtained. We do not yet have demonstrated sensitivity performance values for longer stacked sequences.
As stated above, due to the flat-fielding difficulties as a result of the moving pupil, it appears that best photometric results over the field of view will be obtained with dithered observations.
The most productive dithering schemes will depend on the science goal and size of science targets. For Phase 2, a user-selectable dithering pattern is supported in the PIPT – please see our website for a description of the available dither patterns:
Please note, however, that SALT does not provide fully-automated dithering which makes such observations manual and slightly time consuming. That means, dithering will affect overheads, since every offset will take approximately 30 seconds. Note that the dithering step size is not restricted, but there is a risk of losing the guide star if the step size is large – but see below on the disadvantages of using the auto-guider. If guiding is nevertheless desired, we recommend the total dithering pattern to be constrained within approximately one square arcminute – if larger steps are required, please inform the observer to select a central guide star.
While SALTICAM is equipped with an auto-guider, it has several serious design limitations that limit its overall usefulness:
Because of these shortcomings, we do not advocate the use of the SALTICAM auto-guider during normal imaging. SALTICAM has low read-noise so the sky limit is reached quickly in most broadband filters. Even for U, u′ and H-α it is reached in under a minute. Our current open-loop tracking (Sec 2.4) performance allows unguided exposures of up to 2 minutes which is sufficient for all but the bluest Strömgren filters. Work to improve our open-loop tracking is on-going.
We do support using the auto-guider during slot and frame-transfer mode observations.
Please refer to Sec. 5 for a general description of SALT calibrations. All calibrations should be requested by the relevant check-boxes in the Phase 2 PIPT. The PIPT tool to built observing blocks includes all overheads. For a quick overview of relevant overheads see Sec. 10.
Our current SALTICAM calibrations plan (see below) is based on the specifications of the SALT telescope and our current experience. We would like to highlight the following:
The current SALTICAM calibrations plan for this semester is:
⇨ 5 twilight flats per detector and camera setup
Please note that a larger number of calibrations will need to be justified and we cannot guarantee that these calibrations will be useful.
Currently RSS is routinely being used for the following modes:
For current throughput and sensitivity issues refer to Secs 4.3 and 7.7, respectively. The PIs should be aware that the wavelength ranges predicted by the RSS Simulator currently may have inaccuracies up to +/– 2 nm.
The Robert Stobie Spectrograph (RSS) is the main work-horse instrument on SALT and is a complex multi-mode instrument with a wide range of capabilities. The improved throughput (since 2015, cf. Sec 4.3) together with a well-baffled instrument mean that RSS is a competitive instrument in observations which do not require exceptionally good image quality.
RSS resides at the prime focus, where it takes advantage of the direct access to the focal plane. It was designed to have a range of observing modes, each one remotely and rapidly reconfigurable. In keeping with the overall philosophy of exploiting those areas where SALT has a competitive edge, the instrument has thus several unique, or rare, capabilities:
Since all instruments are available on the tracker at any time, SALTCAM is used for the acquisition images as a slit-viewing camera to ensure that the target is properly positioned in the slit centre and the slit is aligned as desired.
The pixel scale of the detector is 0.1267 arcseconds per unbinned pixel. The positional accuracy and repeatability is currently 0.3” − 0.5” RMS while guiding. Note that there is noticeable fringing in the red narrow-band filters (long-ward of 750 nm) when they are illuminated at discrete wavelengths (while fringing is negligible for broadband illumination). Typical limiting magnitudes are around 20.5 mag − 21.5 mag, depending on the grating. For more details on performance see the individual sections on instrument modes and the RSS commissioning report on the sciencewiki (SALT Web Manager credentials are needed to log in). Technical details are given in the appendix (Sec A.6).
Please use the latest version of the RSS Simulator tool which is an interactive application that allows to select an RSS instrument configuration for an observation based on the most recent throughput model of the instrument and simulated data. It has the ability to simulate the input spectrum for a target and the sky, propagate them through the instrument in spectroscopic mode for a given choice of slit, grating, camera angle, and order-blocking filter, and to calculate the signal/noise per resolution element at the detector given a choice of detector readout parameters.
The detector subsystem comprises a cryostat containing a 3x1 mini-mosaic of CCD chips. The chips are E2V 44-82 CCDs with 2k x 4k x 15 micron pixels. Figure 7.1 shows the layout of the detector with the three CCDs and the slit position indicated. The pixel scale of the detector is 0.1267 arcseconds/unbinned pixel.
Note that the current RSS Simulator has inaccuracies up to ~2 nm in its wavelength range predictions to be noted when assessing the locations of the CCD gaps and edges.
Readout noise for frequently used binning are given in Table 7.1 (more binning combinations are give in the appendix in Sec A.6.
Figure 7.1: RSS detector system with slit position.
Table 7.1: Readout times for the RSS
RSS has a complement of six transmission gratings: one standard surface-relief grating (PG0300) and five volume phase holographic (VPH) gratings — see Table 7.2. VPH gratings have the characteristic that their efficiency varies with input angle (see Fig. 7.1), and thus a single grating can cover a large wavelength range with good efficiency by changing the relative angle between the collimated beam and the grating normal. This is accomplished using a rotating stage. The RSS camera is then articulated to twice the grating angle since the VPH efficiency curve for a given grating angle typically is at a maximum at the Littrow wavelength. The angle of the grating also affects spectral resolution. The higher the value of the grating tilt, the higher the spectral resolving power for a given slit width.
The RSS and VPH grating simulator tools found at
http://astronomers.salt.ac.za/software/ should be used to determine the optimal grating angle and slit-width for an observation. Note also that a feature of VPH gratings is that the resolution and wavelength range of an object depends on the distance of the target from the optical axis. While this is not an issue for long-slit spectroscopy, it will affect multi-object spectroscopy (see Section 7.6.3 for more details).
All gratings are used in first order only. Second-order contamination is removed through the use of order-blocking filters (Sec 7.5).
Wavelength Coverage (nm)
Bandpass per tilt (nm)
Resolving Power (1.25” slit)
Table 7.2: RSS grating complement
Figure 7.1: VPH grating efficiency as calculated using Rigorous Coupled Wave (RCW) analysis in resolving power versus wavelength for a 1.5” slit. The contours correspond to 90%, 70%, and 50%. Wavelength coverage for a few angles is shown for each grating.
Five order-blocking filters are available for RSS spectroscopy: one clear, three UV blocking (with different lower wavelength edges), and one Blue blocking. These filters are listed in Table 7.3 and transmission curves can be found in Sec. A.6.
There are also 40 Fabry-Pérot interference filters which can also be used for the narrow-band imaging; they are listed in Table 7.4. All filter transmission curves are shown in Sec. A.8.
PC03200, PC03400, PC03850
Table 7.3: RSS order blocking filters
Table 7.4: RSS Narrow-band (Fabry-Pérot) Filters
The RSS optical design is not optimized for broad-band imaging (it is recommended to use SALTICAM instead). Narrow-band imaging may be performed with any of the 40 Fabry-Pérot interference filters listed in Table 7.4.
There is considerable fringing in the red narrow-band filters when they are illuminated at discrete wavelengths. Fringing has only been measureable in the narrow-band filters long-ward of 750 nm: with arc lamp illumination (Ne or ThAr), the PI07500 filter shows no fringing while the PI08350, PI08535, and PI08730 filters have obvious fringing at levels of 10–20% peak-to-trough. In all filters tested, fringing is negligible for broadband illumination (sky and QTH lamps) with peak-to-trough variations of 2%.
As with SALTICAM, RSS imaging can be done in frame transfer and slot modes (see Sec 7.6.6).
Long-slit spectroscopy is the most commonly-used mode for RSS.
A variety of slits is available to cover the range of atmospheric seeing conditions expected at the site. The choice of slit widths is driven by considerations of resolution and throughput. The instrument’s slitmask magazine has room for ten tilted longslits, with seven currently available as specified in Table 7.5. All gratings as described in Table 7.4 are available, and all order-blocking filters that are listed in Table 7.3 are also available.
Table 7.5: Available long-slits for RSS
Tracking at the object rates is not commissioned. However, observations of bright targets (that can be seen on the slit) whose motion is aligned along a wide slit (2” or greater) will be accepted. It is the responsibility of the PI to determine the correct position angle to keep the target in the slit and to ensure that the target is bright enough to appear in the slit view images (so that the SALT observer can push it back into the slit if it moves out). For documentation, see
RSS has multi-object spectroscopy (MOS) capability. Slit masks are laser-cut on carbon-fibre masks in Cape Town. A slitmask magazine that has room for 30 MOS masks resides on the instrument, and all fabricated masks are stored on site.
The masks are manufactured following user specifications through a java-based RSS Slit-Mask Tool (RSMT), or a Python-based tool (PySlitmask). The latter is especially useful for optimising slit selections from large catalogs but does not have all the features available in RSMT implemented yet. These tools are downloadable from the SALT proposal tools web pages: http://astronomers.salt.ac.za/software/.
Note that due to the way SALT operates there are restrictions in the available field orientation / Position Angles (PA) for any given RA and DEC, see http://astronomers.salt.ac.za/wp-content/uploads/sites/71/2014/08/SALT_PA_Visibility.pdf for a detailed documentation (beware the crucial distinction between `slit’ and `slot’). Slit masks will be prepared during Phase 2 proposal submission and cut after the Phase 2 submission and checks made by the Liaison SA.
No SALT pre-imaging is required for the mask preparation, provided accurate enough astrometry of the targets is available. We stress that high-quality astrometric solutions in the PI’s images are absolutely crucial for successful MOS observations, that is, 0.3” or better. Pre-imaging can be obtained with SALTICAM if required, though these require their own (time charged) Observing Blocks which have to be observed well in advance of the MOS observations. Pre-existing astrometric files are strongly preferred and the reference stars for alignment and the science slits themselves must come from the same WCS source. MOS masks use 4 – 7 5”x5” holes for reference stars and alignment is done with feedback from through-slit images.
A specific characteristic of the VPH gratings to keep in mind is that the wavelength dependence of the efficiency, as well as the simultaneous wavelength coverage for a given grating setup, depends on the input angle to the grating. In MOS, the light entering through off-axis (in the dispersion direction) slits will hit the grating at different angles. Thus, the efficiency for the off-axis objects will be different than for the on-axis objects. This will in general not be symmetric either. Figure 7.2 illustrates this, and MOS users should consult the VPH grating simulator at
Figure 7.2: Example of the effect of blaze-angle on wavelength range and efficiency in MOS mode. Shown are the default case (on-axis) and the two extreme cases of having an object at the edges of the RSS field-of-view at ±4’ off-axis.
While MOS commissioning as a whole is completed and MOS projects are regularly observed, some telescope design features are placing restrictions on optimal MOS performance. An issue is that field rotation is open-loop on SALT by design (this is to be upgraded in 2018). There is typically a 0.03 degree drift in rotation during a 30 min track around the guide star, which would, at the edge of a field correspond to a spatial drift of 0.25”. Experience has shown however that the rate is not constant, and can be more. An exception are very Southerly tracks where the rotation is at its smallest, and re-alignment is not necessary for at least 1h. For this reason we suggest the following:
A new guider is expected to be installed in March/April 2018 and should be available for the 2018-1 semester, which allow the selection of fainter guide stars and will help with rotational drift, but its performance is as yet not known. PIs are therefore encouraged to plan their observations with our current guider in mind. See section 7.8 for more details
Based on the first semesters of MOS observations the three most frequent issues we have seen when executing submitted programs are:
A set of instructions for preparation of MOS Phase 2 material, including e.g. proper selection of reference stars, can be found from the MOS specific Phase 2 FAQ page at
The SALT RSS Fabry-Pérot system provides two-dimensional imaging spectroscopic capabilities over the whole RSS science field of view (8 arcmin diameter) in the wavelength range 430 – 860 nm with spectral resolutions ranging from 300 – 10000 depending on the mode used and wavelength observed.
The system consists of three etalons with gap spacings of ~0.6 nm, ~2.8 nm, and ~13.6 nm. The etalons are referred to as the low resolution (LR), medium resolution (MR), and high resolution (HR) etalons, respectively. The LR etalon can be used in its normal LR mode or configured as an even lower resolution tunable filter (TF). The MR and HR etalons are designed to be used in conjunction with the LR etalon.
The MR etalon is currently undergoing repairs. Therefore, MR is not available for 2018-1 proposals.
A serious reflection problem between the two inserted etalons was discovered during early commissioning of the dual-etalon modes. Multiple reflections between the etalons introduced a series of ghost images and significantly degraded throughput. A polarising element was inserted between the etalons to remove this and dual-etalon HR is now in regular operations. However, this has cut the flux to a third, which is taken into account in the Simulator.
LR is calibrated for use in the H-α (650–705 nm) and H-β/[O III] (480–515 nm) regions, and dual-mode HR is also calibrated in a narrower H-α region. Further calibrated LR regions are 530–600 and 730–770 nm. Proposals for wavelength regions that are not currently calibrated are also accepted, and PIs are encouraged contact firstname.lastname@example.org as soon as possible so that these calibrations may be scheduled well in advance.
Flexure within RSS significantly impacts Fabry-Pérot calibration, so Fabry-Pérot observations must be carried out as close as possible to a specific telescope rotation angle, which has been fixed to 90 degrees to the parallactic angle for all modes. Therefore, specific positions angles cannot be requested for Fabry-Pérot observations. Because the position angle of the parallactic angle can vary significantly along a track or between east and west tracks it is not possible to predict the location of the CCD gaps a priori.
To maintain maximum flexibility in scheduling we recommend that multiple dithered scans be obtained in cases where the object(s) of interest do not fall completely on the middle CCD.
All available Fabry-Pérot modes need further work on flat-fielding. Flat-fielding is known to be problematic and work is actively ongoing to fully characterize this and how it might be calibrated properly.
Observers should use the tables of etalon free spectral range given in the etalon technical reports and the blocking filter curves to estimate order effects on their particular program. Links to the relevant documentation can be found in the appendix, Sec. A.8.
Polarimetry modes using RSS are (not all all available yet):
We ask that those interested in any unavailable modes should contact email@example.com with their preferences by the same Phase 1 deadline.
The RSS polarimetric optics employs a “wide field” design, in which a polarizing beamsplitter in the collimated beam takes the central half of the field and splits it into two separate orthogonally polarized fields, the “ordinary” (O) and “extraordinary” (E) beams. One (or two) waveplates can be inserted into the beam, right after the field lens in the collimator, to modulate the polarization state with time. The difference between the intensities of the O and E images as a function of time as the waveplates are rotated yields the polarization. For the polarimetric modes, only the central 4-arcminute portion of the focal plane is used (accomplished using a short slit for spectroscopy or a special mask blocking the upper and lower quarter of the field of view for imaging), see Fig. 7.3.
Figure 7.3: FoV for long-slit spectropolarimetry
The waveplate modulators are used in five modes with specific, pre-defined patterns: Linear, Linear-Hi, Circular, Circular-Hi, and All Stokes. For ease of operation, the waveplates are in the same order in all modes, half wave first. Table 7.6 gives the waveplate angle exposure progression pattern for each mode. The angle shown is that between the waveplate optical axis and the beam splitter polarization axis, which is perpendicular to the dispersion direction. A dash (–) means that the waveplate is not inserted.
Table 7.6: RSS Polarimetry waveplate patterns
PIs will need to select a waveplate pattern depending on the nature of the observation:
The full pattern must be completed to yield the stokes parameters.
We give the following advice when planning Phase 1 or defining Phase 2:
For an estimation of expected S/N of linear spectropolarimetric features use the simulator SN prediction (p = 1/SN). For baseline (“instrumental") linear polarization repeatability, assume 0.1–0.2%. This may improve during the semester as more calibration data is obtained, and the analysis software improves. It is very possible that, especially with the VPH gratings (those other than the 300 l/mm), there is a track position dependence of the linear polarization baseline at that level, which is under investigation. If this is of concern, plan on doing everything twice to assess these sort of systematic errors.
As with SALTICAM, RSS imaging can be done in high-speed mode, that is, in frame transfer and slot modes; however, the throughput of SALTICAM is higher and broad-band filters are not available for RSS, making SALTICAM the preferred instrument for imaging observations (unless the narrow-band imaging is required). Timing tests carried out with an independent GPS demonstrate that the absolute and relative timing accuracy of RSS slot mode are good to a few tens of milliseconds.
For details on frame transfer and on slot mode see the relevant modes for SALTICAM (Secs 6.4.2 and 6.4.3, respectively). The minimum exposure times however, differ slightly and are listed in Table 7.7 for the RSS modes (note that software reaction times are not included here).
Frame Transfer and slotmode spectroscopy are only currently available with the 1.5” slit, but please contact the SALT team should you require a different width.
Slot mode (sec)
Frame Transfer (sec)
Table 7.7: Minimum exposure times for Frame Transfer and Slot mode for RSS.
All RSS sensitivity calculations for planning observations should be done with the latest version of the RSS Simulator. PIs are warned that the RSS throughput below 400 nm is not nearly as good as expected originally. See Section 4.3 and Figure 7. for more information. All current information on both the telescope and instrument throughput based on recent measurements is incorporated into the RSS Simulator.
However, we have noticed through experience that PIs often underestimate the required exposure times, especially with fainter targets: Please be conservative when selecting the conditions for the simulation, and remember the IQ and seeing definitions (Secs 4.1 and 3.6.2, respectively) and that seeing and image quality has a large effect on the S/N of targets fainter than sky brightness. In addition, be sure you understand different definitions of S/N (that is, per pixel or per resolution element) and what these mean for your science.
We note that in the past there was straylight reaching the RSS detectors decreasing the S/N of faint observations due to elevated background levels. This issue has long since been fixed and during 2015 we determined that straylight levels are far below the normal night sky levels on RSS. The Sutherland night sky levels were determined to be dark, similar to the Paranal night sky.
As a guideline, approximate magnitude limits at a mid-range wavelength for each grating are tabulated in Table 7.8. The numbers are applicable to long-slit and MOS observations. The magnitude limits have been calculated for 30-min exposures using the 1.5” slit, with 1.3” seeing at zenith, in dark conditions, for an A0V type star (point-source). They correspond to a signal-to-noise ratio of 5 per pixel in 2x2 binning over a 2 x FWHM aperture spectral extraction at the tabulated wavelength.
Central λ (nm)
Mag Limit (V)
Table 7.8: Guideline RSS sensitivities for the central wavelengths of the wavelength ranges of the gratings, for S/N=5 in 30 min exposure. See Fig. 7.1 for available wavelength ranges. The RSS Simulator tool should be used for more detailed calculations.
The RSS auto-guider is routinely used for all RSS observations. Unfortunately, its current sensitivity is limited to rather bright guide stars. The practical limit is V ~ 16 mag with 16.5 mag possible in good seeing. This is usually not a problem for long-slit work, but can be an issue for MOS and Fabry-Pérot where the available field for selecting a guide star may be much more restricted.
The nominal closed-loop tracking performance with a bright guide star is about 0.3” RMS. With fainter guide stars and longer integrations this can degrade to 0.5” RMS.
A major upgrade to the guider is expected to be installed during the shutdown in March/April 2018 with an altogether new system of 2 guide cameras, both of which are more sensitive and will be able to correct for any residual rotational drift or provide auto-focus capability.
Point sources fainter than approximately 21 mag in dark time, and 18 mag in bright time may not be visible to be put on the slit in several second long acquisition images. The exact limit depends greatly on seeing at the time of observation as well as on the diffuseness of the target – the number above relates to point sources in 1.5” to 1.8” seeing. To put fainter targets on the slit, other methods are needed.
Our current positional accuracy and repeatability is currently 0.3” to 0.5” RMS while guiding, measured by performing offsets of sizes varying from 0.5” to 30” and returning to the original position. This accuracy may or may not be sufficient for blind offsetting depending on the science application. If it is enough, e.g. for targeting more diffuse sources, and/or when using wide slits, blind offsetting is operationally feasible and may be requested in an ad hoc manner by discussing it with the liaison astronomer.
In most faint objects cases, however, we recommend providing a brighter alignment object and a PA that will ensure placement of the fainter object in the slit. The PA positioning accuracy is at least 0.5 deg, probably better, so finding a star of V=15–20 mag range at 60” distance would ensure the positioning of the slit with <0.5” accuracy. It is safer to use slit widths of 1.5” or more, and to use alignment stars as close as possible (<60”) to the target.
All of the comments and caveats about SALTICAM dithering that are discussed in Sec. 6.8 apply to RSS as well. The accuracy of the dithering is limited currently to 0.5” RMS. For some purposes (e.g. Fabry-Pérot), this is perfectly fine. For others (e.g. dithering blindly between different slit positions), it may not be. However, since in most cases an object will be visible on the slit-viewer, the observer just would re-check alignment before re-starting exposures (60 sec overhead is defined for dithering along the slit, which includes the move and tweak of position if required).
Nod-and-shuffle mode is not offered during 2018-1 due to it not being commissioned.
Please refer to Sec. 5 for a general description of SALT calibrations. All calibrations should be requested by the relevant check-boxes in the Phase 2 PIPT. The PIPT tool to built observing blocks includes all overheads. For a quick overview of relevant overheads see Sec. 10.
The RSS calibration plan (see below) is based on the SALT telescope specifications and on current experience. We would like to point out the following:
The calibration plan (see Sec. 5 for definitions) for RSS for the upcoming semester is:
HRS is available and routinely being used in all of its modes (LR, MR, HR and HS) but with one default detector configuration: 1x1 binning, single amplifier, slow readout. See Sec. 8.4.1 for a brief discussion on mode availability.
The SALT HRS is a dual-beam (blue: 370–555 nm, and red: 555–890 nm) fibre-fed, white-pupil, échelle spectrograph, employing VPH gratings as cross dispersers. The cameras are all-refractive. The concept is for SALT HRS to be an efficient single-object spectrograph using pairs of large (350 μm to 500 μm; 1.6–2.2 arcsec) diameter optical fibers, one for source (object) and one for background (sky). Some of these feed image slicers before injection into the spectrograph, which deliver resolving powers of R ~14000 (unsliced 500 μm fibres), ~40000 (sliced 500 μm fibres), and ~65000 (sliced 350 μm fibres). A single 2k x 4k CCD is sufficient to capture all the blue orders, while a 4k x 4k detector, using a fringe-suppressing deep-depletion CCD, is used for the red camera. Complete free spectral ranges are covered by both the blue and red arms. The spatial resolution is ~0.3 arcseconds. The accuracy of HRS radial velocities is at least 200 m/s for low resolution mode and 150 m/s for medium and high resolution modes.
The blue arm has an e2v CCD 44-82 blue detector which is thinned and back illuminated. It has a broadband anti-reflective coating applied. The pixel format is 2048x4096 (15μm pixels). The red arm has an e2v CCD 231-84 with 4096 x 4096 pixels (15μm pixels). This chip is manufactured from deep depletion silicon and has the Extra Red Plus fringe suppression option. The fringe suppression process attenuates the internal interference fringes seen at long wavelengths (>800nm) on thinned, backside illuminated CCDs.
The quantum efficiency of the red CCD is 93.1% at 650 nm, falling to 58.4% at 900nm. For the blue CCD it is 90% at >500 nm and dropping off to ~74% at 400 nm.
HRS supports a variety of detector read-out modes, with users able to tailor read-out speed, binning and the number of read-out amplifiers to suit their needs. Modes and read-out speeds are summarized in Tables 8.1 and 8.2 below.
1000kHz and 400kHz read-out speeds are supported on both detectors. The former offers a shorter read-out time at the expense of marginally higher read-out noise. 1000kHz should offer acceptable read noise performance in many circumstances (the values in Table 8.1 are averaged over all two/four read-out amplifiers for blue/red CCDs, respectively).
CCD binning options are 1x1, 2x2, 3x3, 8x8 and 3x1 (that is, binning in the spatial direction only). 1x1 binning is the standard binning mode, since binning will degrade spectral resolution in all but the low resolution mode (where a resolution element is multiple pixels in width). Despite no binning in the spectral direction, the 3x1 binning mode will still cause some resolution loss in all but the low-resolution mode, since it will smear the effect of line tilt across the order. The advantages of binning are reduced read-out times and reduced read-out noise, since fewer ‘pixels’ are read-out.
It is possible to read-out the detectors using single or multiple read-out amplifiers. For the 2k x 4k blue CCD, the options are one or two amplifiers. In the case of the larger 4k x 4k red CCD, the options are one or four read-out ports. Read-out speed scales with the number of amplifiers (so four amplifier read-out is four times faster than a single amplifier at the same speed and binning). Note that when using multiple read-out amplifiers, each area of the chip will have a different bias level and overscan region, which must be dealt with in data reduction.
Note that the HRS CCDs are read-out in series rather than in parallel, as parallel read-out can cause a small cross-talk signal between the detectors. The blue CCD is therefore read-out before read-out of the red CCD commences. Read-out times reflect the sum of the two read-outs. As an example, running three back-to-back iterations of 10s exposures using the standard detector settings would take 3 x (10s + 23s + 37s) = 210s.
Table 8.1: HRS red and blue detector read-out noise with different read-out speeds.
Table 8.2: HRS red (top) and blue (bottom) detector read-out times (in seconds) with different binning and read-out amplifier configurations. The default (=standard) readout mode is highlighted.
Users are strongly advised, in almost all cases, to use the standard detector configuration as indicated in Table 8.2 for HRS proposals. Although it is the slowest option, the data quality will be of the highest achievable standard, with the simplest possible data reduction requirements. SALT will provide the calibration files (weekly CalSys arcs and flats for all modes; daily HS internal ThAr mode arcs; daily bias frames, see Sec. 8.9.2). This mode is also currently the only one which is fully supported by the data reduction pipeline. Users using other modes will only receive the raw data and will have to process the data themselves.
Alternatively, in extreme and specialist circumstances, users may request a configuration other than this default read-out option. In order to accommodate such a request, additional calibration frames in the requested new custom read-out mode will have to be created in addition to the standard ones. Clearly it is unfeasible to offer every possible read-out configuration (there are 20 possible read-out mode combinations per detector), as the calibration requirements would be vast. It will be thus the responsibility of the PI to provide a detailed and valid technical motivation.
As an example, a hypothetical proposal with one target, one visit and 2x1800s exposures on a bright star in low-resolution mode, might prefer to use multiple amplifiers, 1000 kHz read-out speed and 3x3 binning. SALT would not support such a request merely to save the proposer 117s of read-out time at 3600s of observing time.
On the other hand, a hypothetical proposal with 40 visits of 3x2s exposures for, e.g., an exoplanet monitoring program could make a reasonable argument to use a 1000 kHz read-out configuration. Since overheads make up the bulk of the time in this case (a reduction from 7200s to 3480s overheads for 240s observing time), AstOps may consider granting such a request at their discretion. Another good example is a scientific requirement for high time-resolution observations requiring low read-out overheads.
Although an 8x8 binning option is available for HRS, the various gains in 8x8 mode for each CCD amplifier have not been empirically determined yet. For this reason, in addition to those mentioned above, 8x8 binning should be avoided until proper detector characterisation has been obtained.
SALT HRS offers four different operational modes, which vary in spectral resolution at the expense of instrument throughput. Table 8.3 summarizes the four modes along with their characteristics and options.
Low Resolution Mode
Medium Resolution Mode
High Resolution Mode
High Stability Mode
Fibre Diameter (μm)
Fibre Diameter (arcsec)
Blue arm resolution
Red arm resolution
Blue arm transmission (total %) at 460nm*
Red arm transmission (total %) at 625nm*
Fibre mode scrambling
Nod and shuffle
Total photon count***
Table 8.3: Summary of HRS mode characteristics and efficiency predictions.
* These efficiency values represent the as-measured ‘end-to-end’ throughput for the spectrograph as a whole, including the optical fibre feed.
** Note that the Iodine cell and simultaneous ThAr feed cannot be used simultaneously.
*** From an exposure meter (unless using the optional internal ThAr lamp in simultaneous use in the high stability mode).
This is lowest resolving-power R = 14000 configuration. The configuration offers the same fibre input diameter as the R = 40000 (MR) mode (that is, 500 μm) but with the benefit of a 1.4× higher throughput because the fibre output is not image-sliced (hence the coarser resolution).
Examples, where the lowest resolving power may be tolerable and where the improved background sampling might be beneficial, include spectroscopy of diffuse interstellar bands against lines of sight to distant stars or quasars and molecular band analyses of stars in Local Group galaxies.
The R = 40000 mode is the most commonly used SALT HRS mode. It has adequately high resolving power for many projects but with a larger fibre diameter and higher throughput than the R = 65000 (HR) mode. Studies of objects whose intrinsic line widths are broader than two resolution elements of the R = 65000 mode, such as rotating stars (e.g. most O and B stars), stars in which the Balmer line strength measurements are the principal aims, and studies of molecular bands at medium resolution are likely to benefit from the resolving power versus throughput trade-off available in this mode.
The R = 65000 mode is useful only for those projects for which the lower throughput compared to the R = 40000 mode is more than offset by the greater resolving power. Such observing projects include studies of line profiles in investigations of stellar atmosphere dynamics, resolving closely spaced lines, or the study of absorbing structures in the interstellar or intergalactic medium at the highest velocity resolution. Studies that benefit from fine sampling of the stellar line profiles, such as the most precise radial velocity work, will also utilise this resolving power. Recall, however, that the wavelength stability of the instrument as a whole will be much higher than in traditional non-vacuum spectrographs, and astronomers may find they can achieve adequate velocity accuracy even at R = 40000 because of the improved systematics compared to other spectrographs.
The high stability mode is optimised for precision radial velocity measurements and is implemented at R = 65000, because of the importance of adequately sampling the line profiles in order to achieve sub-resolution-element accuracy (an error of 5 ms-1 corresponds to 10-3 of a resolution element). The light path in this mode includes a permanent ‘double scrambler’ to improve the radial scrambling of the optical fibres and reduce the spectral shifts due to the star moving on the input face of the fibre. In this mode it is also possible to place an iodine cell into the beam (both channels) to provide a superimposed set of wavelength reference lines in the 500–620 nm range, or to illuminate the second (sky) fibre with an internal Th-Ar calibration source to obtain a simultaneous wavelength calibration. The efficiency of this mode is therefore expected to be ~50% – 70% of the normal high resolution mode and would normally only be used where this level of wavelength stability is essential. It should be noted that the iodine cell has yet not been fully characterised (i.e. no Fourier Transform Spectrometer spectra are available, only the commonly available generic iodine atlases). It should also be noted that the simultaneous ThAr and iodine cells may not be used together.
Figures 8.1 and 8.2 illustrate the echellogramme maps of the red and blue arm spectra as they appear on their 4k x 4k and 4k x 2k detectors respectively. The cross-over wavelength between the two arms is at 555 nm, with the blue arm covering 370–555 nm and the red detector covering 555–890 nm.
Figure 8.1: Wavelength coverage for the red arm of SALT HRS. Key spectral features are noted on each image, as are order numbers and the blaze wavelengths λB.
Figure 8.2: Wavelength coverage for the blue arm of SALT HRS. Key spectral features are noted on each image, as are order numbers and the blaze wavelengths λB.
The standard HRS data pipelines (MIDAS and pyHRS, see http://astronomers.salt.ac.za/software/hrs-pipeline/ for more details) make use of the daily and weekly obtained calibration files (see Sec. 8.8.2). A Velocity Standard (RVST) star, observed in all HRS modes, is similarly reduced, and its velocity is measured and compared with the velocity from the RV catalogue. As shown in http://www.saao.ac.za/~akniazev/pub/HRS_MIDAS/HRS_stability.pdf, the accuracy of HRS radial velocities is at least 200 m/s for LR mode and 150 m/s for MR and HR modes for this scheme of library calibrations. As an example, our study for MR mode is shown in Fig. 8.3, where all library calibrations were done during the same night.
Figure 8.3: The comparison of measured velocities with their catalogue values for RV standards obtained with the MR mode over two months. The difference between the calculated velocity and velocity from the catalogue for each spectrum is shown with black dots. 1-sigma errors are shown with bars. The calculated average value for the total sample is shown with the horizontal long dash line (blue color for the blue arm, red for the red arm and black for blue+red arms) and 1-sigma errors for the total sample are shown with green long dash lines.
We also studied the stability of the RV determination versus the difference in days between the date of observation and date of other library calibrations. An example from such a study is shown Fig. 8.4. The top panel shows the difference between the calculated velocity and the catalogue velocity versus the difference in days between the date of observation of the RVST and the date of other library calibrations. The weighted averages for many measured stars is shown together with the calculated error.
Figure 8.4 also shows that for MR mode both blue and red arm data do not show any obvious systematics if calibrations were done not on the same day but within 5–7 days of the observation. It is thus easy to get an accuracy of less than 150m/s using both arms’ data or only the red arm.
Figure 8.4: The comparison of measured velocities with their catalogue values for RV standards obtained with HRS MR mode depending on the time (in days) between calibrations and science observations. The calculated average value for the total sample, as described in Fig. 8.3, is shown with horizontal lines. In this case it is coincident with Delta Days = 0. The weighted average of the calculated difference between measured velocity and velocity from the catalogue are shown for each date.
Figures 8.4 and 8.5 show the anticipated SNR ratio of SALT HRS as a function of stellar visual magnitude (mv). Note the difference in performance of the four instrument modes due to variance in throughput. These values are currently based on predicted instrument efficiencies (see below for on-sky comparisons). Users may simulate HRS observations using the simulator tool available at http://astronomers.salt.ac.za/software/.
Figure 8.5: The expected signal to noise ratio (S/N) of SALT HRS as a function of stellar visual magnitude (mv) using the red instrument arm and a variety of operational modes. The calculations are for a wavelength of 725 nm and the low (R~14000), medium (R~40000) and high (R~65000) spectral resolving powers. A blackbody object with surface temperature of 5500K, 2 arcsec FWHM seeing at the fibre input, exposure time of 1800 sec and a telescope airmass of 1.3 are assumed. The sky brightness is calculated assuming the moon to be at first quarter. The S/N is for each extracted half-resolution element at the échelle blaze peak.
Figure 8.5: The expected signal to noise ratio (S/N) of SALT HRS as a function of stellar visual magnitude (mv) using the blue instrument arm and a variety of operational modes. The calculations are for a wavelength of 460 nm and the low (R~14000), medium (R~40000) and high (R~65000) spectral resolving powers. A blackbody object with surface temperature of 5500K, 2 arcsec FWHM seeing at the fibre input, exposure time of 1800 sec and a telescope airmass of 1.3 are assumed. The sky brightness is calculated assuming the moon to be at first quarter. The S/N is for each extracted half-resolution element at the échelle blaze peak.
We have verified that bright object (V = 6–10 mag) throughput is consistent with the simulator tool predictions. Due to the on-sky size of the fibres, it is possible to observe faint targets with HRS but there are several indications that for the faintest targets (V > 16), the simulator overestimates the signal to noise ratio. Thus PIs are urged to be conservative in planning fainter target HRS observations, and should carefully consider observing targets fainter than V=18 even with the LR mode.
Please refer to Sec. 5 for a general description of SALT calibrations. All calibrations should be requested by the relevant check-boxes in the Phase 2 PIPT. The PIPT tool to built observing blocks includes all overheads. For a quick overview of relevant overheads see Sec. 10.
Our current HRS calibrations plan (see below) is based on the specifications of the SALT telescope and our current experience. We would like to highlight the following:
SALT HRS is equipped with an exposure meter, which is available for use in all four operational modes (with the exception of the high stability mode when the simultaneous internal ThAr lamp is in use). Time-indexed photon counting data should therefore be available, as well as flux-weighted mid-points for the exposures.
The calibration plan (see Sec. 5 for definitions) for HRS for the upcoming semester is:
BVIT is available this semester. Currently, the FoV is fixed at 1.9 arcminutes diameter.
The Berkeley Visible Image Tube camera (BVIT) is a visitor instrument built at the Space Science Laboratory of the University of California-Berkeley. It is a photon-counting camera with a ~1.9 arcmin diameter field of view, capable of very high time resolution (millisec or microsec) photometry with a B, V, R or H-alpha filter. It can be used for objects with magnitudes ranging from V~12–20 mag. BVIT is available for general use. The most accurate and up-to-date information about the instrument, as well as a count-rate estimator, can be found at: http://bvit.ssl.berkeley.edu/.
BVIT does not provide high-precision absolute photometry; however, by observing nearby standard stars, a flux intensity relative precision of ~ 5% can typically be obtained. Every detected photon is assigned a time of arrival and a (x,y) position on the detector, which allows an observer a high degree of post-acquisition data analysis flexibility.
At this time, we are not allowing the BVIT iris size to be altered. The field of view is thus fixed at ~1.9 arcmin in diameter. Note that the two constraints when using BVIT are the global and local count rates. The global rate (sum of all counts on the detector) cannot exceed 1MHz. The local counts from any single source cannot exceed 100 kHz. If proposing, please carefully check the field and consider counts from all sources that will be exposed and not solely the target of interest.
A 1500s overhead on BVIT data allows for acquisition from one of the larger field-of-view facility instruments (SALTICAM or RSS) as well as an acquisition and count rate check from BVIT.
Due to the complexity of the instrument setup, all BVIT observations will be carried out by our local BVIT expert, thus observations are also subject to expert availability.
No calibrations are needed for BVIT.
All SALT Phase 1 proposals must include the overhead times associated with the science observations in the proposed time. The most accurate way to estimate overheads is to use the PIPT tool to build actual Observing Blocks to see how long their execution times are. While Block preparation is not required at Phase 1, the exercise is strongly encouraged to check how feasible the science observations are regarding track times and Block limitations (see Sec 2.6) when overheads are included. The main sources of overheads are summarised in Table 10.1 to give PIs an idea of the involved times. PIs must be especially aware that in addition to pointing and acquisition related overheads, there may be calibration related overheads. The latter may or may not be charged for (see sections on the Calibration Plans for the individual instruments), and may or may not affect the available time for science during a track time (e.g. arcs taken after an observation vs. arcs in-between observations).
Please note especially that the basic acquisition time including pointing, focusing, object acquisition, and guidance configuration is 1500s for BVIT, 900s for RSS–MOS, 600s in all other RSS modes as well as SALTICAM, and 500s for HRS.
The overheads for arcs depend strongly on the setup, and for blue and/or high resolution setups can take several minutes. You should check the PIPT for the overhead estimates.
Acquisition (all modes)
point, acquire, (guide). Includes need for re-focusing in longer blocks.
with ~0.5” accuracy
8 - 14
depending on filter position
Readout, Full Frame, Slow
9.0, 21, 53
for binning 6x6, 2x2, 1x1
Readout, Full Frame, Fast
8, 14, 26
for binning 6x6, 2x2, 1x1
Readout: Frame Transfer
minimum exp.times apply
Readout: Slot Mode
minimum exp.times apply
point, acquire, guide, RSS config
point, acquire, guide, RSS config
point, acquire, guide, RSS config
point, acquire, guide, RSS config
re-acquisition, RSS config
Full RSS config change
Grating angle change
71, 42, 142
100￮ → 0￮, 50￮ → 0￮, 100￮ ⇄ 0￮
Nod along slit, blind offset
60 (spectroscopic dither),
30 (imaging dither)
with ~0.5” accuracy
Calibration screen in
Calibration screen out
check in PIPT
minimum 60 sec + readout time, cal.sys already inserted
5 frames, lamp change, cal.sys already inserted
Readout Full Frame, Slow
7, 18, 28, 51
4x4, 2x2, 1x2, 1x1
Readout Full Frame, Fast
6, 11, 14, 24
4x4, 2x2, 1x2, 1x1
Readout: Frame Transfer
minimum exp.times apply
Readout: Slot Mode
minimum exp.times apply
Acquisition (all modes)
point, acquire, guide, configure HRS
e.g. high stability mode with simultaneous ThAr to HS mode with iodine cell
Full readout and file saving overhead in Default HRS Mode
Readout Red Frame, Slow, Single Amplifier
6, 11, 13, 37
3x3, 2x2, 3x1, 1x1
Readout Red Frame, Fast, Single Amplifier
4, 6, 7, 19
3x3, 2x2, 3x1, 1x1
Readout Red Frame, Slow, Quadruple Amplifier
2, 3, 4, 10
3x3, 2x2, 3x1, 1x1
Readout Red Frame, Fast, Quadruple Amplifier
1, 2, 2, 5
3x3, 2x2, 3x1, 1x1
Readout Blue Frame, Slow, Single Amplifier
5, 8, 8, 23
3x3, 2x2, 3x1, 1x1
Readout Blue Frame, Fast, Single Amplifier
3, 4, 5, 10
3x3, 2x2, 3x1, 1x1
Readout Blue Frame, Slow, Double Amplifier
3, 4, 5, 12
3x3, 2x2, 3x1, 1x1
Readout Blue Frame, Fast, Double Amplifier
2, 2, 3, 5
3x3, 2x2, 3x1, 1x1
Acquisition (all modes)
point, acquire, configure
Table 10.1: SALTICAM, RSS, HRS, BVIT overhead estimates.
* See Sec. 8 for a fuller explanation of HRS read-out times
ADC = atmospheric diffraction corrector
BVIT = Berkeley Visible Image Tube camera (Sec 9)
CCD = charge-coupled device
Co-I = Co-Investigator
COM = commissioning proposal program (Sec 3.3.4)
DC = default calibration (Sec 5)
DIMM = Differential Image Motion Monitor (Sec 3.6.2)
DDT = director’s discretionary time (Sec 3.3.3)
FoV = field of view (8’x8’)
FP = Fabry-Pérot (RSS mode; Sec. 7.6.4)
FWHM = full width half maximum
HR = high resolution mode (Sec 8.5.3)
HRS = high resolution spectograph (Sec 8)
HS = high stability mode (Sec 8.5.4)
IQ = image quality (Sec 4.1)
LC = library calibration (Sec 5)
LR = low resolution mode (Sec 7.6.4 (FP) and 8.5.1 (HRS))
LS = long-slit RSS mode (Sec 7.6.2)
LSA = liaison SALT Astronomer (assigned to a proposal and thus the first point of contact for any queries regarding that proposal)
LSP = large science program (Sec 3.3.2)
MLT = multi (that is, long-term proposal program, Sec 3.3.1)
MOS = multi-object spectrograph (RSS mode, Sec. 7.6.3)
MR = medium resolution mode (Sec 8.5.2)
PA = position angle
PC = Principal Contact (Sec 3.7)
PI = Principal Invesigator
PSF = point spread function
PIPT = proposal and observation preparation tool (Sec 3.7)
RSMT = RSS slit-mask tool (Sec 7.6.3)
RSS = Robert Stobie Spectrograph (Sec 7)
SA = SALT astronomer (observer)
SAC = spherical aberration corrector
SALT = Southern African Large Telescope
SAMS = SALT array management system: active mirror alignment system (Sec A.3)
SALTICAM = SALT Imaging Camera (Sec 6)
SCI = science program (Sec 3.3.1)
SNR = signal-to-noise ratio
SO = SALT operator
TF = tunable filter narrow-band imaging (FP) mode (Sec 7.6.4)
ToO = target of opportunity (Sec 3.9.1)
TTT = Too Tight Track syndrome (Sec 2.5)
UCC = user-requested charged calibrations (Sec 5)
UNC = user-requested non-charged calibrations (Sec 5)
VPH = Volume Phase Holographic (Sec 7.4, A.6)
VPHG = VPH transmission gratings (Sec 7.4, A.6)
Acquisition images: Used to set up the observation, locate guide stars, check FOV etc. (Sec 2.6)
Astro Ops: Astronomy Operations (email firstname.lastname@example.org) at SALT, South Africa
Burst mode: Mode or the primary mirror where each mirror segment forms an independent image of the observed object (Sec 4.3)
Charging: Charging time (as in allocated time by the TAC) (Sec 3.1.1)
Closed loop: Guidance mode ON (normal operations mode; Sec 2.4)
Fried parameter r0: standard measure of atmospheric turbulence, in centimeters; it is mainly affected by small temperature variations and depends on wavelength; by default λ = 500 nm (Sec 3.6.2)
Observing Block: minimum schedulable unit (Sec 2.6)
Open loop: Guidance mode OFF (e.g., for SALTICAM imaging; Sec 2.4)
Optional targets: Actual observing targets can be taken from a pool of `optional’ targets to increase likelihood of observing (Sec 3.5)
Phase 1: Proposal phase to apply for observing time (Sec 3.7)
Phase 2: Proposal phase to prepare observations once time has been allocated (Sec 3.9)
Priority classes: determines placement in the observing queue (Sec 3.4)
Pupil: View of the mirror as the tracker sees it; only light reflected from this pupil reaches the instruments. Note that the pupil changes over an observation, that is, track (Sec 2.4)
SALT Web Manager: Interface to the proposal and executed observations (Sec 3.7)
Too Tight Track syndrome: only a very short time window within which the SALT Astronomer can point to the target to obtain the track length required – if this window is missed, the block has to wait for the next available window (Sec 2.5)
Track length/time: the time a target can be tracked without moving the telescope (Sec 2.5)
Visibility: the time a target is visible to SALT (Sec 2.5)
American Museum of Natural History
American Museum of Natural History, USA
Dartmouth College, USA
Inter-University Centre for Astronomy & Astrophysics
Inter-University Centre for Astronomy & Astrophysics, India
[all Polish Institutions]
[all South African institutions]
Rutgers University (also State U. of New Jersey), USA
UK SALT Consortium
University of North Carolina
University of North Carolina – Chapel Hill, USA
University of Wisconsin-Madison
University of Wisconsin-Madison, USA
Table A.1: Time on SALT is allocated by share-holding. However, in addition to the current share-holders, Durham University (UK) is currently receiving observing time due to its building the HRS instrument, and Göttingen University (GER) and University of Canterbury (NZ) who recently have withdrawn from the partnership, are also still receiving some observing time.
The SALT mirror comprises 91 hexagonal segments figured to have spherical surfaces with a radius of curvature of 26.165 m. When all segments are pointing to a common focus, they act as a 10-m spherical mirror. The mirror segment mounts are supported on a steel truss that expands and contracts as the temperature increases or decreases, carrying the segments with it. There are 3 actuators attached to each segment that provide the ability to change its pointing direction. The actuator displacements correct for two effects, one being the supposed uniform change in shape of the truss, the other being any random change due to irregular expansion or contraction or to electronic effects in the sensing circuitry.
SAMS is an acronym for the SALT Array Management System. It comprises a set of sensors mounted on the mirror segments connected to racks of electronics feeding data to a Labview program that is designed to maintain the overall shape of the SALT mirror array once it has been set up with the CCAS instrument.
Before the implementation of SAMS, after approximately 2 hours of observing astronomical targets or when the image quality from the full array had deteriorated, the telescope structure was rotated to point at CCAS, a few measurements were made of the state of the central 7 segments and then science observing resumed. Less than 1 hour of the night over and above the time taken for the usual two to three realignments of the full array was thus spent on monitoring.
Today, SAMS continuously maintains the primary mirror figure and with it the focus, so that the image quality has significantly improved and does not change with time anymore. See http://www.salt.ac.za/news/sams-project/ and Gaijar et al. 2016 on how the mirror alignment and SAMS work in detail.
Unlike conventional telescopes, SALT’s primary mirror is stationary during an observation. The only movement occurs at the prime focus, as the tracker, carrying the prime focus payload, migrates across the primary mirror. The light-collecting area of the telescope’s mirror, known as the entrance pupil, is represented in the diagrams below as the yellow coloured circle. Only the mirrors inside the circle collect starlight. The diagrams also show the centrally obscured mirror segments and the shadow of the tracker.
Figure A.1: When the tracker is centred (4), the telescope has its greatest light-collecting area, making it equivalent to a 9-m telescope. Even when the tracker is at its maximum off-axis position (1, 6), SALT is still equivalent to a 7-m telescope.
Figure A.2 shows the payload at the prime focus of the telescope without the tracker structure (cf. Fig. 2.2). The SAC is the grey cylinder at the bottom of the payload. At the top of the payload the RSS instrument with the camera is visible. The right-hand panel in Fig. A.3 shows a zoom-in with the covers removed: The slitmask holder (green) and grating holder (yellow) are visible. The whole camera can rotate on the structure, depending on the articulation angle.
Figure A.4 shows the three instruments underneath the RSS: SALTICAM (orange), HRS (green, to tef left of SALTICAM), and BVIT (grey, to the right of SALTICAM). The folding mirrors (grey with a red holder) are shown opposite SALTICAM, they direct the light coming from the SAC into the respective instrument. The SAC is shown underneath the instruments in green grid and yellow lense holder. Figure A.5 shows the SAC with blue ray tracing.
Figure A.2: The payload in the focal plane.
Figure A.3: The RSS instrument at the top of the payload.
Figure A.4: SALTICAM (orange), HRS (green, to the left of SALTICAM), and BVIT (grey, to the right of SALTICAM). The folding mirrors (grey with a red holder) are opposite SALTICAM. The SAC is shown underneath the instruments in green grid and yellow lense holder.
Figure A.5: SAC with ray tracing (blue) and focal plane indicated at the top.
See the SALTICAM optical design, Figure A.6. 0.3 arcsec (EE50), combined with SALT 0.6 arcsec (EE50), to give 0.67 arcsec image quality, independent of seeing. EE80 shall be no more than 0.5 arcsec. Distortion shall be less than 1 per cent. The mean plate scale shall be 107 micron/arcsec or 9.35 arcsec/mm within 1 per cent.
Science Field of View
8 arcmin in diameter
Guide Star Field of View
10 arcmin in diameter
320 – 950 nm
8 position filter unit. Available filters include U, B, V, R, I, clear; Sloan u', g', r', i', and z'; Strömgren u, v, b, y, H-beta wide, H-beta narrow, and red extensions SRE1, SRE2, SRE3, and SRE 4; H-alpha; neutral density; and short wavelength interference filters at 340 nm (FWHM 35 nm) and 380 nm (FWHM 40 nm). (see the PIPT for filter curves)
E2V Technologies 44–82
2048 x 4102 x 15 micron square pixels per chip
Imaging area per chip
30.7 x 61.5 mm2 imaging area per chip
2 readout amplifiers per chip
2 x 1 mini-mosaic
better than 99.99%
164 and 172 k e-/pix (for CCDs SALT-01 and SALT-02 respectively)
less than 1e-/pix/hr at 160 K
less than 3.0 e-/pix at 100 kHz (10.0 usec/pix) (slow readout)
SDSU II (Leach) from Astronomical Research Camera Inc.
Thinned, back-illuminated. Deep depletion silicon.
Astro Broad Band anti-reflection coating.
NOTE: CCD-01 (aka CCD-B) is on the right side of the default SCAM display view and written SALTICAM files and CCD-02 (aka CCD-A) is on the left.
Delivered quantum efficiency for each chip is shown below:
NOTE: CCD-01 (aka CCD-B) is on the right side of the scam view and written SCAM files and CCD-02 (aka CCD-A) is on the left.
Delivered cosmetics for each chip are shown below:
Gain is user selectable and dependent on selected readout speed:
1 x 1 to 9 x 9, independently in each direction
Frame transfer architecture: 0.10 sec frame transfer time 100–333 kHz (10–3.0 usec/pix). Observer specifies readout speed as "FAST" or "SLOW".
Full frame, fast readout:
Full frame, slow readout:
See https://wiki.salt.ac.za/index.php/SCAM_overheads for details.
Minimum exposure times:
The table shows the minimum exposure times for slot mode and frame transfer mode for all the valid binning parameters:
Up to 10 windows (prefer not to specify for P-V phase)
Fastest windowed photometry:
0.1 sec/sample with no dead time
Please use the most recent version of the SALTICAM simulator (http://astronomers.salt.ac.za/software/) for the most accurate exposure times and corresponding signal-to-noise ratios.
The lens system reduces the SALT f/4.2 prime focal ratio to f/2, thereby enabling the full 8-arcmin diameter science field of view, as well as almost all of the guide star field of view, to be captured on the 2x1 CCD mosaic. The lenses are made from UV-transmitting crystals, and the CCDs have excellent UV performance, so the instrument is expected to be very efficient at short wavelengths. The optical design is illustrated in Fig. A.6.
Figure A.6: SALTICAM optical path.
Figure A.7 shows the fields of view superimposed on the detector and includes:
Figure A.7: SALTICAM full layout.
The detector is a 2x2 mosaic of 2kx4kx15 micron pixel CCD 44–82 chips from E2V Technologies. These devices are thinned, back-illuminated and coated with the E2V Astro Broad Band coating. They are also deep-depletion devices for better near-infrared sensitivity and lower fringing. A schematic of one of the chips is shown in Fig. A.8 (O'Donoghue et al 2004).
Figure A.8: SALTICAM schematic for one of the two CCDs.
For moderate time resolution on the order of a few sec, Frame Transfer (FT) operation is used. This is explained by the left hand diagram in Fig. A.9: a mask (shown in grey) covers the lower half of each chip. At the end of each exposure, the image in the top half of the chip is rapidly (200 millisec) shifted to the lower half where it is readout while the next image in the top half accumulates during the next exposure.
Figure A.9: SALTICAM schematic for frame transfer (left) and slot mode (right). The gray regions are masked.
Figure A.10. SALTICAM schematic for slot mode readout.
Even faster sampling can be obtained with so-called slot mode: in this mode a mask is advanced over the entire chips except for a slot just above the frame transfer boundary. Instead of half frame transfers at the end of each exposure, 144 rows are moved and this allows exposure times as short as 100 millisec. The slot position is illustrated in the right hand diagram in Fig. A.9. Figure A.10 shows a schematic of the slot mode readout: Panel (a) shows the situation at the end of exposure n in one of the 4 amplifiers of the SALTICAM CCDs. The 144 rows indicated are transferred in about 15 millisec over the frame transfer boundary which is supposed to be aligned with the lower edge of the slot. At the end of this operation (Panel (b)), exposure n lies in the 144 rows below the FT boundary, and exposure n+1 begins. During exposure n+1, the 144 rows next to the readout register (indicated by exposure n-2 but in reality n-6) are read out, and the other data sections slowly scroll down by 144 rows. At the end of exposure n+1, the situation is then as in panel (c) which is the same layout as in panel (a) except that n is now replaced by n+1. See also O'Donoghue et al 2004.
Of course both FT mode and slot mode techniques require field of view to be sacrificed for time resolution: in FT mode, half the field of view is lost; in slot mode, only the slot is available for imaging. The intended use of slot mode is to position a rapidly varying target star and a brighter nearby companion star in the slot to perform differential photometry of the variable with respect to the comparison star. The telescope rho stage can be rotated to locate comparison stars at arbitrary position angles within the slot.
"Typical" instrument and system efficiencies are shown in Fig. A.11 and were calculated for the on-axis field position using:
The SALTICAM efficiency (black line) is the product of the optics (blue) and the CCD (red) curves. For reference, RSS performance taken from Fig. 5 of the PFIS PDR Instrument Description Document is shown in green.
Figure A.12 shows the overall expected efficiency based on:
See O'Donoghue et al 2003 for details.
Figure A.11: SALTICAM instrument efficiency with PFIS (now RSS) for comparison.
Figure A.12: SALTICAM overall efficiency (including telescope optics and atmosphere).
RSS is an all-refractive collimator and camera system, optimized for spectroscopic performance in the 320-900 nm wavelength range. The collimator has 9 lenses in 5 groups plus a fold mirror before the last doublet. In the 150 mm diameter collimated beam are the shutter and the dispersers, which include one of six gratings (five volume phase holographic (VPH) gratings and a standard transmitting surface relief grating) or a double-etalon Fabry-Perot system. The camera (F/2.2, 8.6 arcsec/mm) has 9 lenses in 4 groups, with the final lens, a field flattener, being the dewar window. All optical surfaces are spherical except for the first surface in the camera, which is an asphere.
The collimator is designed to work in the 320-1700 nm range, to accommodate a future near-infrared camera. Air-glass interfaces in the collimator will be coated with either a MgF2/Solgel hybrid or just a MgF2 antireflection coating. Camera surfaces will be coated with a MgF2/Solgel hybrid or multi-layer antireflection coating.
To compensate for image error introduced by possible differences in filter thicknesses and uncompensated thermal effects, the camera will have an active focus system. Focusing will be accomplished by moving the singlet and the triplet in the camera together. Additionally, the camera will need to be refocused for each configuration, as the imaging was not optimized for all wavelengths simultaneously. However, a fixed focus position can be set for each configuration. Then final focus error due to filters/thermal effects can be removed.
Figure A.13 shows the main part of the RSS instrument and Fig. A.14 shows the optical path.
Figure A.13: RSS instrument. SALTICAM is located at the bottom of the image. Dark blue rays are shown being focused onto the first lense. The grating holder is shown in bright yellow, and the slitmask magazine holder in green. The whole left hand section rotates on the dark blue track, depending on the articulation.
Figure A.14: Top: technical diagram of RSS; bottom: RSS optical path.
The detector subsystem comprises a cryostat containing a 3x1 mini-mosaic of CCD chips. The chips are E2V (formerly Marconi) 44-82 CCDs with 2k x 4k x 15 micron pixels. The mosaic is housed in an evacuated cryostat and thermally connected to the cold end of a Cryotiger, which cools the chips sufficiently to render dark current insignificant while minimizing QE reduction. The detectors are managed by an SDSU III CCD controller, which is in turn controlled by a PC. Figure A.15 shows the detector layout and the position of the slit. Readout speeds for various selected binnings and two readout modes are given in Table A.1. Note that horizontal and vertical binning result in different readout speeds, e.g., 2x1 (fast) takes 9.8 sec, while 1x2 (fast) takes 12.0 sec.
Table A.1: Readout speeds for FAST and SLOW readout modes for the RSS
Figure A.15: RSS detector system with slit position.
The VPH (volume phase holographic) gratings provide high diffractive efficiency and significantly reduced scattered light as compared to standard surface-relief gratings. Also, VPH gratings can be tuned to shift the diffraction efficiency peak to a desired wavelength. The use of such gratings requires the camera to be able to articulate, to accommodate various grating tilts. The grating resides on a rotatable stage, and the entire camera articulates about the same axis as the grating rotation, so that the grating is always used in a Littrow configuration.
Mechanical limitations require that the camera angle is quantized to every 0.75 degrees, with a maximum articulation of 100 degrees. Thus, a finite (but still large) number of camera positions are available. The camera angle determines the central wavelength on the detector, with longer wavelengths associated with larger camera articulation angles.
The three UV filter transmission curves are shown in Fig. A.16 and the Blue filter transmission curves are shown in Fig. A.17.
Figure A.16: UV filter transmission curves. Only the filters UV-32 (PC03200), UV-34 (PC03400) and UV-38 (PC03850) are available.
Figure A.17: Transmission curve for Blue filter PC04600.
RSS has multi-object spectroscopy capability. Slitmasks are fabricated using a laser cutting machine and inserted into a magazine that resides on the instrument. The magazine can carry 30 of these customized slitmasks at any given time. User designed slitmasks will be cut in Cape Town and stored on site with a unique bar code for identification.
One specific characteristic of VPH gratings to keep in mind is that the wavelength dependence of the efficiency depends on the input angle to the grating. In multi-object spectroscopy, the light entering through off-axis (in the dispersion direction) slits will hit the grating at different angles. Thus, the efficiency for the off-axis objects will be different than for the on-axis objects. This will in general not be symmetric either, i.e. objects that are at +2 arcminutes off-axis will have a different wavelength dependence of the efficiency from those at -2 arcminutes off-axis.
Additionally, the wavelength coverage on the detector for off-axis objects will be different than that for on-axis. So, the simultaneous wavelength coverage for a given grating setup with a multi-object slit mask will depend on how far off-axis the objects are.
Figures A.18 demonstrates these effects. The two plots show, for the G3000 grating at 50 degrees grating angle, what the wavelength coverage and efficiency for the on-axis and two off-axis positions is. Note that for the full field (4 arcminutes off-axis) the simultaneous wavelength coverage is reduced and the efficiency can be as much as 50% lower for certain wavelengths.
Figure A.18: Wavelength coverage and efficiency for the on-axis and two off-axis positions at +/- 2’(top panel) and +/- 4’ (bottom panel).
The SALT RSS Fabry-Pérot system provides spectroscopic imaging over the whole RSS science field of view (8 arcmin diameter) in the wavelength range 430–860 nm with spectral resolutions ranging from 300–10,000. Figure A.19 shows the layout of the instrument.
The system employs a set of three etalons with gap spacings of ~6, ~28 and ~136 µm respectively. The etalons are referred to as the small gap (SG), medium gap (MG) and large gap (LG) etalons respectively. The SG etalon may be selected on its own for use in tunable filter (TF) and low resolution (LR) modes. The MG or LG etalon are selected for use in medium resolution (MR) and high resolution (HR) mode respectively. Both these etalons are always used in conjunction with the SG etalon which effectively acts as a transmission filter in this case.
A set of 40 blocking filters are employed to select the transmission order. Filter transmission curves are shown below.
Table A.2 summarises the key characteristics of the system in the various modes.
Figure A.19: RSS optical path with Fabry-Pérot
430 – 860 nm
430 – 860 nm
430 – 860 nm
430 – 860 nm
Free Spectral Range at 650 nm
Resolution at 650 nm
Finesse at 650 nm
Effective plate gap
<1Å / hour
<1Å / hour
<1Å / hour
Table A.2: Characteristics of the FP system
A detailed description of the system is given in the paper by Naseem Rangwala, Ted Williams and their collaborators (2008);
Additionally, Ted Williams has produced an introduction to Fabry-Pérot on SALT.
The following 3 etalon reports detail the technical details and performance of each etalon:
Tables containing the FWHM of the spectral resolution, the resolution and free spectral range of each etalon as a function of wavelength are included in each report. This information is helpful for proposal planning.
For the filter characteristics see Table 7.4; the transmission curves are shown in Figure A.20.
Figure A.20: Filter transmission curves for the FP narrow-band filters.
The HRS is situated at the prime focus along with the other instruments, see Fig. A.4 the green coloured instrument to the left of SALTICAM. The instrument’s optical path is shown in Fig. A.21.
Figure A.21: Optical path for the HRS.
There are two cameras for the HRS, one for the blue arm (comprising 8 lenses and a clear aperture of 150mm), the other for the red arm (comprising 6 lenses and a clear aperture of 170mm). Both cameras have a cylindrical field flattening lens as the last element which has been made removable such that it can also act as the window for the detector cryostats.
The cameras were tested in double pass transmission (at 633nm) with an autocollimating flat mirror across the field of view of the cameras. Table A.3 gives the results. The wavefront error (WFE) for the cameras alone was found by subtracting the expected aberrations computed in Zemax from the measured performance.
WFE (on axis)
WFE (on axis)
0.44λ RMS (λ=633nm)
> 85 % at 380nm
> 88.5% at 410nm
> 92% above 450 nm
Table A.3: Summary of camera tests
More Details on the HRS can be found here:
SALT Proposal Info: 2018 Semester 1