The 1.3-m telescope was previously the 2MASS southern telescope before SMARTS took over its operation. A permanently-mounted, dual-channel, optical-IR imager called ANDICAM takes simultaneous optical and infrared data on the SMARTS 1.3-m telescope. The 1.3-m is operated entirely in service / queue mode.
ANDICAM has been in regular operations at the 1.3-m since February 2003 by the SMARTS Consortium. Previously, it had been operated in queue mode on the 1.0-m (YALO Consortium) with the optical detector since the 1998B semester. The IR array was installed in July 1999, enabling simultaneous optical and infrared imaging, including dithering in the IR channel while the optical channel integrates. ANDICAM was constructed by the Ohio State astronomical instrumentation group led by Darren DePoy and its construction was funded in part by the National Science Foundation.
ANDICAM takes simultaneous optical and infrared data by using a dichroic with a CCD and a HgCdTe array. A moveable mirror allows dithering in the IR while an optical exposure is going on. The primary purpose of the instrument is for microlensing event follow-up to look for the presence of planets and other anomalous behaviour. ANDICAM is operated by the Prospero control software. It also has a twin--DANDICAM (Dutch ANDICAM)--that is used on a 1m telescope in South Africa. With ANDICAM one can obtain UBVRIJHK photometry within a 6 arcmin (optical) or 1 arcmin (near-IR) field.
| FILTER | Plot | Data file | |
| CCD Filters | KPNO-B | kpno_b.pdf [4] | kpno_b.txt [5] |
| KPNO-V | kpno_v.pdf [6] | kpno_v.txt [7] | |
| KPNO-I | kpno_i.pdf [8] | kpno_i.txt [9] | |
| Infrared Filers | J-band | andi_j.pdf [10] | j_andi.txt [11] |
| H-band | andi_h.pdf [12] | h_andi.txt [13] | |
| K-band | andi_k.pdf [14] | k_andi.txt [15] | |
| Legacy Filters | YALO B | yalo_b.pdf [16] | b_yalo.txt [17] |
| YALO wide R | yalo_r.pdf [18] | r_yalo.txt [19] |
Telescope Operator Instructions [21]
Optical Processing Procedure [35]
Reports and Logs
Nightly 1.3m Observing Log Archive [23]
1.3m Nightly Observer's Reports [24]
1.3m Telescope Trouble Reports [36]
Report Forms
Photometric Standards and Measurements Reports [37]
Nightly Observing Logs [38]
Nightly Observing Reports [21]
Daily Processing Reports [25]
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March 2009
To assist you in reducing your infrared images, we are now providing combined infrared flat field images for each filter. These are created by combining all of the flat images that are taken at each dither position, producing one flat image for each filter. These can be downloaded from the ftp site in /home/ftp/pub/smarts13m/flatsir.
Separate flat field images (at each of the dither positions) will continue to be available from the same ftp directory as before (/home/ftp/pub/smarts13m/calibsir).
Please direct any questions to either Michelle Buxton or Suzanne Tourtellotte.
If you have to generate schedules for a telescope (or anything else) and are interested in streamlining the process, we recommend the software developed at NASA Goddard by the Science Goal Montior (SGM) group. The main website can be found here and you can download the specific software developed for SMARTS here. Email Michelle Buxton if you need help with creating the specific sun and moon files needed (this is currently done using another piece of software, XEphem).
The 1.3m/ANDICAM now has neutral-density filters installed for viewing bright sources in V, I, H, and narrowband He 1038nm. Tests with standard stars show that the V+ND combination has an attenuation of 4.6 (a factor of 39,000, or 11.5 magnitudes) over that of the V filter, and the I+ND combination an attentuation of 3.0 (1100, or 7.6 magnitudes).
The ANDICAM instrument has two optical neutral density filters, V+ND4 and I+ND4, and two infrared neutral density filters, H+ND4 and 10830+ND3. (The 10830+ND3 filter is a narrowband He filter.) The optical ND filters are 5-arcminute diameter round filters, and the IR ND filters are 2.4-arcmin square filters. According to the previous paragraph, the V+ND filter has an attenuation of 4.6 (a factor of 39,000, or 11.5 magnitudes) over that of the V filter, and the I+ND combination has an attenuation of 3.0 (1100, or 7.6 magnitudes).
From observations of Eta Car in the ND4 filters done by Alan Whiting, the FWHM generally ranges from 2.5 to 4.9 pixels in V. He also notes that flat fields taken through the attenuated filters have not been successful in calibrating the data. However, the flats from the unattenuated V, I, and H filters seem to work fine with ND filter observations.
We have spotted a peculiarity in observing the Landolt standard PG1323. It appears as though the light of a bright star (most likely Spica) outside the field of view is not properly baffled, causing the raised level of the background, as shown here:
In principle, this should not affect the count rate in the standard stars themselves, but, we do not recommend using this particular standard for your observations.
The 1.3m has been removed from the CTIO exposure time calculator. The values obtained using this calculator were found to be too optimistic by several orders of magnitude. Please estimate you exposure times using the values found at the ANDICAM detector website (http://www.astronomy.ohio-state.edu/ANDICAM/detectors.html#sens [39]).
PLEASE NOTE: The U filter is currently broken and unusable.
SMARTS optical images are processed with the IRAF task CCDPROC using a bias prepared with the IRAF task ZEROCOMBINE and a domeflat or skyflat prepared with the IRAF task FLATCOMBINE. As of November 1, 2006, the SMARTS optical images are processed slightly differently. In order to remove the low-level horizontal "banding" that we have seen at times during the last six months, the overscan is now fit with a cubic spline function of order 11. All other steps remain the same. The old processing parameters can be found here.
Modified 11/01/2006
===============================================================================
Ten biases are taken each night and are combined into a single
bias frame using the IRAF task ZEROCOMBINE.
The IRAF task ZEROCOMBINE parameters are set as follows:
|
I R A F Image Reduction and Analysis Facility |
|||
| PACKAGE = ccdred | |||
| TASK = zerocombine | |||
| input = | List of zero level images to combine | ||
| (output = | ZERO) | Output zero level name | |
| (combine= | average) | Type of combine operation | |
| (reject = | minmax) | Type of rejection | |
| (ccdtype= | ) | CCD image type to combine | |
| (process= | no) | Process images before combining? | |
| (delete = | no) | Delete input images after combining? | |
| (clobber= | no) | Clobber existing output image? | |
| (scale = | none) | Image scaling | |
| (statsec= | ) | Image section for computing statistics | |
| (nlow = | 1) | minmax: Number of low pixels to reject | |
| (nhigh = | 1) | minmax: Number of high pixels to reject | |
| (nkeep = | 1) | Minimum to keep (pos) or maximum to reject(neg) | |
| (mclip = | yes) | Use median in sigma clipping algorithms? | |
| (lsigma = | 3.) | Lower sigma clipping factor | |
| (hsigma = | 3.) | Upper sigma clipping factor | |
| (rdnoise= | 0.) | ccdclip: CCD readout noise (electrons) | |
| (gain = | 1.) | ccdclip: CCD gain (electrons/DN) | |
| (snoise = | 0.) | ccdclip: Sensitivity noise (fraction) | |
| (pclip = | -0.5) | pclip: Percentile clipping parameter | |
| (blank = | 0.) | Value if there are no pixels | |
| (mode = | ql) | ||
===============================================================================
VRI dome flats are observed every night, 10 exposures of each.
JHK dome flats are observed every third night in rotation. 10 exposures are taken at each of the 7 dither positions (dither throw = 40). 10 additional exposures at each dither position are then taken with the dome lamps off. The final flat at each dither position is the difference between the combined lamp-on flat minus the combined lamp-off flat.
B sky flats are taken due to undesirable artifacts present in the B domes. A minimum of 3 images are taken every night weather permitting. It is required that individual skyflats have different RA and
DEC values.
In all cases, the individual flats are processed first with CCDPROC for the overscan and zero corrections, then combined with FLATCOMBINE.
FLATCOMBINE parameters are set as follows for the SKY flats:
|
I R A F Image Reduction and Analysis Facility |
|||
| PACKAGE = ccdred | |||
| TASK = flatcombine | |||
| input = | List of flat field images to combine | ||
| (output = | FLAT) | Output flat field root name | |
| (combine= | median) | Type of combine operation | |
| (reject = | minmax) | Type of rejection | |
| (ccdtype= | ) | CCD image type to combine | |
| (process= | no) | Process images before combining? | |
| (subsets= | no) | Combine images by subset parameter? | |
| (delete = | no) | Delete input images after combining? | |
| (clobber= | no) | Clobber existing output image? | |
| (scale = | mode) | Image scaling | |
| (statsec = | ) | Image section for computing statistics | |
| (nlow = | 1) | minmax: Number of low pixels to reject | |
| (nhigh = | 1) | minmax: Number of high pixels to reject | |
| (nkeep = | 1) | Minimum to keep (pos) or maximum to reject(neg) | |
| (mclip = | yes) | Use median in sigma clipping algorithms? | |
| (lsigma = | 3.) | Lower sigma clipping factor | |
| (hsigma = | 3.) | Upper sigma clipping factor | |
| (rdnoise = | 0.) | ccdclip: CCD readout noise (electrons) | |
| (gain = | 1.) | ccdclip: CCD gain (electrons/DN) | |
| (snoise = | 0.) | ccdclip: Sensitivity noise (fraction) | |
| (pclip = | -0.5) | pclip: Percentile clipping parameter | |
| (blank = | 0.) | Value if there are no pixels | |
| (mode = | ql) | ||
FLATCOMBINE parameters are set as follows for the DOME flats:
|
I R A F Image Reduction and Analysis Facility |
|||
| PACKAGE = ccdred | |||
| TASK = flatcombine | |||
| input = | List of flat field images to combine | ||
| (output = | FLAT) | Output flat field root name | |
| (combine= | average) | Type of combine operation | |
| (reject = | crreject) | Type of rejection | |
| (ccdtype= | ) | CCD image type to combine | |
| (process= | no) | Process images before combining? | |
| (subsets= | no) | Combine images by subset parameter? | |
| (delete = | no) | Delete input images after combining? | |
| (clobber= | no) | Clobber existing output image? | |
| (scale = | mode) | Image scaling | |
| (statsec= | ) | Image section for computing statistics | |
| (nlow = | 1) | minmax: Number of low pixels to reject | |
| (nhigh = | 1) | minmax: Number of high pixels to reject | |
| (nkeep = | 1) | Minimum to keep (pos) or maximum to reject(neg) | |
| (mclip = | yes) | Use median in sigma clipping algorithms? | |
| (lsigma = | 3.) | Lower sigma clipping factor | |
| (hsigma = | 3.) | Upper sigma clipping factor | |
| (rdnoise= | 6.5) | ccdclip: CCD readout noise (electrons) | |
| (gain = | 2.3) | ccdclip: CCD gain (electrons/DN) | |
| (snoise = | 0.) | ccdclip: Sensitivity noise (fraction) | |
| (pclip = | -0.5) | pclip: Percentile clipping parameter | |
| (blank = | 1.) | Value if there are no pixels | |
| (mode = | ql) | ||
===============================================================================
Images are processed, one filter type at a time, with a bias and a skyflat of the corresponding filter type using the IRAF task CCDPROC. The result is a processed image, prefixed with the letter "r", that have been OZF'ed (overscanned, flattened and zeroed) but not T'ed (trimmed).
When biases are not taken for a given night, the ZEROCOMBINEd bias from the nearest available night is used instead. This bias will have already gone through CCDPROC with images of its same night. The bias section for use in overscanning was determined by IMPLOT to extend from less than 3 and more than 14, so [3:14,1:1024]) was chosen as the overscan strip image section.
When contemporaneous skyflats are not available, FLATCOMBINEd skyflats from previous nights are used instead. These skyflats will have already been processed using their own contemporaneous biases.
The IRAF task CCDPROC parameters are set as follows:
I R A F
Image Reduction and Analysis Facility
PACKAGE = ccdred
TASK = ccdproc
|
I R A F Image Reduction and Analysis Facility |
|||
| PACKAGE = ccdred | |||
| TASK = ccdproc | |||
| images = | @in.(filtertype) ) | List of CCD images to correct | |
| (output = | @out.(filtertype) ) | List of output CCD images | |
| (ccdtype= | ) | CCD image type to correct | |
| (max_cac= | 0) | Maximum image caching memory (in Mbytes) | |
| (noproc = | no) | List processing steps only? | |
| (fixpix = | no) | Fix bad CCD lines and columns? | |
| (oversca= | yes) | Apply overscan strip correction? | |
| (trim = | no) | Trim the image? | |
| (zerocor= | yes) | Apply zero level correction? | |
| (darkcor= | no) | Apply dark count correction? | |
| (flatcor= | yes) | Apply flat field correction? | |
| (illumco= | no) | Apply illumination correction? | |
| (fringec= | no) | Apply fringe correction? | |
| (readcor= | no) | Convert zero level image to readout correction? | |
| (scancor= | no) | Convert flat field image to scan correction? | |
| (readaxi= | line) | Read out axis (column|line) | |
| (fixfile= | ) | File describing the bad lines and columns | |
| (biassec= | [3:14,1:1024]) | Overscan strip image section | |
| (trimsec= | ) | Trim data section | |
| (zero = | ccd(night).bias) | Zero level calibration image | |
| (dark = | ) | Dark count calibration image | |
| (flat = | ccd(night).sky/domeflat(filter) ) | Flat field images | |
| (illum = | ) | Illumination correction images | |
| (fringe = | ) | Fringe correction images | |
| (minrepl= | 1.) | Minimum flat field value | |
| (scantyp= | shortscan) | Scan type (shortscan|longscan) | |
| (nscan = | 1) | Number of short scan lines | |
| (interac= | no) | Fit overscan interactively? | |
| (functio= | spline3) | Fitting function | |
| (order = | 11) | Number of polynomial terms or spline pieces | |
| (sample = | *) | Sample points to fit | |
| (naverag= | 1) | Number of sample points to combine | |
| (niterat= | 1) | Number of rejection iterations | |
| (low_rej= | 3.) | Low sigma rejection factor | |
| (high_re= | 3.) | High sigma rejection factor | |
| (grow = | 0.) | Rejection growing radius | |
| (mode = | ql) | ||
General-purpose photometric standards are observed every photometric night on the 1.3m telescope.
The procedure is as follows:
Each photometric night, 1 Landolt field is observed ONCE in all optical filters. In addition, 2 IR standards (one blue and one red) are observed ONCE in all IR filters. Because extinction coefficients cannot be calculated on such nights, "default" values (see below)are used for calculations of zeropoints and color terms.
Periodically, more thorough observations of the same standards are performed, observing each of the 3 standard fields (1 Landolt, 2 IR fields) at 3 different airmasses in order to calculate extinction coefficients. The medians of these values, taken over many months, are the "default" extinction coefficients mentioned above.
Standard star images are available to all users and are not charged against their allocation. We do our best to choose those Landolt fields with at least 3 standard stars available in the field of view. If your program requires additional standard observations, please include them in your PhaseII submission. Additional observations are charged against your allocation.
| Photometric Results | Optical [43] | Infrared [44] | |
| Extinction Coefficients Values | Optical [45] | Infrared [46] | |
| Description of Photometric Calculation Methods | Optical [47] | Infrared [48] |
Links:
[1] http://www.astro.yale.edu/smarts/observing.htm
[2] http://www.astro.yale.edu/smarts/ANDICAM/data.html
[3] http://www.astronomy.ohio-state.edu/ANDICAM/detectors.html
[4] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/kpno_b.pdf
[5] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/KPNO_B.txt
[6] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/kpno_v.pdf
[7] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/KPNO_V.txt
[8] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/kpno_i.pdf
[9] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/KPNO_I.txt
[10] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/andi_j.pdf
[11] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/J_andi.txt
[12] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/andi_h.pdf
[13] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/H_andi.txt
[14] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/andi_k.pdf
[15] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/K_andi.txt
[16] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/yalo_b.pdf
[17] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/B_YALO.txt
[18] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/yalo_r.pdf
[19] http://www.ctio.noao.edu/noao/sites/default/files/instruments/filters/R_YALO.txt
[20] http://www.astro.yale.edu/smarts/ANDICAM/mail.html
[21] http://www.astro.yale.edu/smarts/smarts13m/observer.html
[22] http://www.astro.yale.edu/smarts/smarts13m/optprocessing.html
[23] http://www.astro.yale.edu/smarts/ANDICAM/ObsLogs/
[24] http://www.astro.yale.edu/smarts/ANDICAM/Reports/Nightly/
[25] http://www.astro.yale.edu/smarts/smarts13m/procreps.html
[26] http://www.ctio.noao.edu/noao/content/13-m-photometric-standards
[27] http://www.astro.yale.edu/smarts/smarts13m/pg1323.html
[28] http://www.astro.yale.edu/smarts/smarts13m/ndfilters.html
[29] http://www.astro.yale.edu/smarts/smarts13m/queue.html
[30] http://www.astro.yale.edu/smarts/usage/usage13m2004b.dat
[31] http://www.astro.yale.edu/smarts/usage/usage13m2005a.dat
[32] http://www.astro.yale.edu/smarts/usage/usage13m2005b.dat
[33] http://www.astro.yale.edu/smarts/usage/usage13m2006a.dat
[34] http://www.astro.yale.edu/smarts/usage/usage13m2006b.dat
[35] http://www.ctio.noao.edu/noao/content/optical-processing-procedure
[36] http://www.astro.yale.edu/smarts/ANDICAM/Reports/Trouble/
[37] http://www.astro.yale.edu/smarts/ANDICAM/Reports/
[38] http://www.ctio.noao.edu/noao/content/SMARTS-Logs
[39] http://www.astronomy.ohio-state.edu/ANDICAM/detectors.html#sens
[40] http://www.ctio.noao.edu/noao/content/13-m-telescope
[41] http://www.ctio.noao.edu/noao/sites/default/files/telescopes/smarts/tele13/optprocessing.txt
[42] http://www.ctio.noao.edu/noao/content/smarts-contacts
[43] http://www.astro.yale.edu/smarts/smarts13m/photrepsCCD.html
[44] http://www.astro.yale.edu/smarts/smarts13m/photrepsIR.html
[45] http://www.astro.yale.edu/smarts/smarts13m/ext.coeffsCCD
[46] http://www.ctio.noao.edu/noao/sites/default/files/telescopes/smarts/tele13/ext.coeffsIR
[47] http://www.ctio.noao.edu/noao/content/13-m-smarts-photometric-calibrations-bvri
[48] http://www.ctio.noao.edu/noao/content/13-m-SMARTS-Photometric-Calibrations-JHK