0Assigned ID: 2105
----- Attempting Submission 1 (Fri Apr 09 18:44:19 GMT 2021) -----
HST Phase I Proposal 2105 successfully submitted.
Receipt: # 2105-1Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).
Guiding Tolerance is not allowed when Gyro Mode is not a 3-Gyro mode (3GFHST or 3GOBAD).This re-re-re-submission follows the approval of HOPR 92866. It repeats 1 orbit of visit18 that failed
because the guide stars were not acquired.-134689626----- Attempting Submission 1 (Thu Jul 29 18:32:09 GMT 2021) -----
HST Phase II Proposal 16772 successfully submitted.
Receipt: # 16772-1
----- Attempting Submission 2 (Mon Aug 09 18:44:19 GMT 2021) -----
----- Attempting Submission 3 (Mon Feb 28 21:06:42 GMT 2022) -----
----- Attempting Submission 4 (Wed Mar 09 15:35:26 GMT 2022) -----
----- Attempting Submission 5 (Wed Aug 03 16:13:29 GMT 2022) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 6 (Tue Aug 13 14:41:22 GMT 2024) -----The errors refer to visits that have already been carried out or failed. As such they do not impat the new visit, which checks out fine.They Pack a Punch: Mechanical Feedback by the Lowest-Luminosity AGNsLINER nuclei, the long-lived, low-accretion-rate states of supermassive black holes, are critical for understanding the AGN phenomenon in the context of galaxy evolution. Observations have established the presence of black-hole related activity in most LINERs. But, we have also learned that the line emission on ~1" (~100 pc) scales, used for LINER classification with ground-based data, is not balanced by the radiative energy output of the nucleus alone. Another, unknown power source provides most of the power on these scales. The leading candidate is centrally-driven outflows of gas that carry at least as much power as the radiative luminosity of the AGN and produce optical emission lines through shock heating. Past HST case studies of four LINERs have spatially resolved the line-emitting regions, suggested a transition from photoionization on scales of tens of pc to shock excitation on larger scales, and allowed estimates of the kinetic power. Thus, LINERs may be signposts of feedback from the AGN onto the host galaxy. As such, they help us understand more distant, important objects. But a larger, truly representative sample, spanning a wider range of LINER AGN properties, is needed to test and generalize those results. We propose optical spectroscopy, spatially resolving ~0.1 arcsec scales, for a diverse and representative sample of 15 LINERs. We have designed an economical observing program by exploiting spectra available in the archive for a large fraction of the targets. We will carry out the first comprehensive mapping and exploration of the excitation of LINER gas using multi-dimensional line-ratio diagrams on scales of ~10 pc.PRACTICAL GOALS AND GENERAL SCIENTIFIC STRATEGY
This program will study a sample of 15 galaxies with LINER nuclei using archival and new STIS spectra. The primary scientific goal is to test models for the excitation of line-emitting gas. For each object we need STIS long-slit spectra with the G430L and G750M gratings in order to measure a variety of emission-line ratios along the slit as a function of distance from the nucleus. This means that the slit orientation must be the same (modulo 180 deg) for the G430L and G750M observations. Moreover, we need the slit to be narrow (0.1-0.2 arcsec) so as to get the best possible spatial resolution.
For the sample of 15 galaxies, the right combination of STIS spectra exists in the archive for 6 cases (no new observations are needed for these 6 objects). There are 5 other cases for which we will obtain either G430L or G750M spectra along a slit direction that matches an observation already in the archive (for these 5 objects we need to place the slit at a specific position angle, modulo 180 deg). For the remaining 4 objects no suitable data are available in the archive so we will get a complete set of G430L and G750M spectra (for these 4 objects any slit position angle is fine as long as it is the same for the G430L and G750M observations).
SCIENCE EXPOSURE TIMES
To estimate science exposure times we used measurements from published papers and archival spectra. We assumed that the Balmer line strengths decline by factors of 10 and 100 at 12 and 40pc from the nucleus, respectively, and set the nuclear strengths according to the G750M H-alpha flux of each galaxy; for galaxies without a G750M spectrum, we normalized first to a galaxy that had one and then according to the ground-based measurement of H-alpha. We assumed typical ratios of H-alpha/H-beta~3 and [SII]/H-alpha>0.6 (essential in testing shock models). We took archival spectra as templates and scaled them according to the above. With the STIS ETC we found the exposure times needed to achieve a S/N=60 at the peak H-beta in nuclear spectra (continuum included), giving S/N=20 in the integrated H-beta flux after continuum subtraction at 12pc from the nucleus (or S/N=5 at 40pc). The S/N in the [OII]3727 line will be similar or higher, while that of [OIII]5007 will depend on how steeply its strength declines with distance from the nucleus. Past studies show that upper limits on weak lines are still quite useful for the proposed tests.
TARGET COORDINATES
Since 7 of the 9 targets in this program have been observed before with STIS (long-slit spectroscopy) we looked up the coordinates from those observations in the HST archive, checked them, and then adopted them. To vet the coordinates we examined the observing sequences and phase II proposals of those past programs as well as the archival spectra themselves. We selected the coordinates corresponding to the science exposure that followed acquisition, checking for any slit offsets. In one case (M84) the slit was offset by 0.1 arcsec from the target after acquisition (perpendicular to its direction) so we are adopting the same offset here to match the slit position exactly. We documented the program numbers and other relevant details in the visit notes for each object.
For two targets (NGC4438 and NGC4457) we did not find any past HST observations that we could use so we turned to other sources for the coordinates. For NGC4438 we adopted the coordinates of the compact nuclear radio core detected with the VLA (this coincides with a resolved H-alpha source detected with WFC3 imaging at FWHM=0.3 arcsec). For NGC 4457 we adopted the coordinates of the galaxy nucleus from SDSS DR13, which agree to 0.2 arctic with the 2MASS coordinates and to 0.04 arcsec with the coordinates of the unresolved nuclear X-ray source detected by Chandra. We documented all the relevant details and references to relevant published papers in the visit notes of these two objects. As a last step we examined finding charts of the targets made with the APT target confirmation tool.
SLIT POSITION ANGLE
For 5 targets in our program we are obtaining a new G430L or G750M long-slit spectrum to complement an archival spectrum. In these cases we need the same slit width as the archival observation. We also need the slit position angle in the new observation to match that of the archival observation to +/- 3 degrees. If this tolerance is exceeded the slit positions will not overlap at distances < 5 arcsec from the galaxy nucleus, which will compromise our ability to compare spectra from different observations. We thus determine the ORIENT parameter for the new observation following the instructions in section 6.2.2 in the Phase II Proposal Instructions. We document these requirements and our calculation of the ORIENT parameter in the visit notes as appropriate.
TARGET ACQUISITION AND DITHERING
Since 7 of the 9 targets in this program have been observed before with STIS (long-slit spectroscopy) we looked up the acquisition procedures used by those programs and adopted them or adapted them. The target acquisitions are carried out with the MIRROR+F28X50LP. The targets are elliptical galaxies or bulges of spirals but a few of them have prominent nuclear point sources (the others also have bright centers because of centrally-concentrated line emission). For 3 targets (NGC1097, M84, M104) that are known to have a nuclear point source we use ACQTYPE=POINT. For all other targets we use ACQTYPE=DIFFUSE with CHECKBOX=3 and FLUX-CENTROID.
For 3 targets (M89, M104, M94) we are using the 0.1 arcsec slit in order to match the archival observation, hence we must follow the initial acquisition with a peak-up acquisition. For the other targets a peak-up acquisition is not needed since we are using the 0.2 arcsec slit.
We also looked up the acquisition exposure times for the previously observed targets and compared them with new estimates we made with the acquisition ETC in order to determine suitable acquisition exposure times for this program. In our ETC calculations we assumed a spectrum of an elliptical galaxy (since most of our targets are ellipticals and the others are bulges of spirals) and we scaled it according to the flux density measured in past STIS observations. In the calculations for ACQTYPE=DIFFUSE we assumed a source size of 2 arcsec. For 2 targets that do not have archival STIS spectra we scaled the flux densities of published, ground-based spectra using scale factors determined from objects that have both ground-based and STIS spectra available. In most cases we found that, the acquisition exposure times from the ETC were longer than that those in the archival observations. We always adopted the longer of the two exposure times and made sure that they are very far from the saturation limits returned by the ETC.
To mitigate the effects of charge-transfer inefficiency, we place the galaxy nucleus at the recommended E1 aperture position at 5 arcsec from the end of the slit.
To mitigate the high rate of hot pixels in the STIS CCD we will dither the exposures along the slit. We adopt a 3-step dither pattern with 0.15 arcsec per step, which we have used successfully in the past in program 12595, that was very similar to this program.
DISTRIBUTION OF EXPOSURES INTO ORBITS AND VISITS
We constructed visits of 3 orbits or less.
For 3 targets (NGC3607, NGC4438, NGC4457) for which we are taking both G430L and G750M (3 and 2 orbits, respectively) we have broken up the observations with different gratings into separate visits. But these visits require the same slit position angle, hence they can be combined into a single visit, if that is more convenient.
For 2 objects (M84 and M95) we have broken up long, 5-orbit exposures with the same grating into two separate visits. These visits can be executed at any time as long as they have the same slit position angle. The can be combined into single visits, if that is more convenient.
IMPACT OF REDUCED-GYRO OPERATIONS
Reduced-gyro operations will primarily impact the schedulability of our observations. Since 5 of our 9 targets need to be observed with a particular slit position angle, the number of available observing windows is limited. To help with the scheduling flexibility, we have constructed visits that are 1-3 orbits in duration. We also note that variability of the spectra is not a cause for concern for this program, since we are observing regions with a large physical size. Therefore, the visits can be spread out over a long period of time and they need not be carried out in any particular order (although different visits of the same target should have the same slit position angle).
DUPLICATIONS
We will get a duplicate G430L spectrum of NGC 4374. The new spectrum will have the same slit position angle as the existing G750M spectrum of this object and a much higher S/N, as needed for our goals.
Similarly we will get a duplicate G430L spectrum of NGC3507 because the existing spectrum has a very poor S/N that is not adequate for our goals. The requested exposures are >3 times longer than the archival ones.
We will also get duplicate G750M spectrum of NGC1097. Although there are G750M spectra in the archive, these were taken with the slit at a different position angle than the existing G430L spectrum. Although a G750L observation at the same slit position angle as the G430L observation does exist in the archive, it has very low spectral resolution and the lines of interest (H-alpha+[NII] and the [SII] doublet) are blended together. The new G750M observation will match the slit position angle of the archival G430L observation and will have a high enough spectral resolution to resolve and separate the emission lines of interest.M. Eracleous, D. Maoz, A. J. Barth, L. C. Ho and J. C. Shields have extensive expertise in the physics of LINERs. They have studied the UV and optical spectra and images of LINERs, their energy budgets, the X-ray and radio properties of their weak AGNs, and the kinematics and dynamics of the gas in the nuclei of AGNs in general and LINERs in particular. They have been principal authors of many of the papers that led up to this proposal. They have also authored, both separately and in collaboration with each other, papers on physical models for the power source of LINERs. Relevant to this program, they all have extensive technical expertise in optical and UV spectroscopy and imaging. Moreover, M. Eracleous has worked extensively on absorption-line spectroscopy of quasar outflows.
M. Molina has extensive experience in analyzing the spatially resolved spectra of LINERs with the HST and ground-based IFU spectra of star-forming and dwarf galaxies. This experience includes calibrating the spectra, modeling and decomposing the continuum, measuring the emission lines, and comparing the measurements with models. She was the lead author of the paper that presents the case studies and the analysis methods on which this proposal is based (Molina et al. 2018, ApJ, 864, 90). She is now leading a program that studies accretion onto massive black holes in dwarf galaxies and associated feedback processes.
J. C. Runnoe has a great deal of technical expertise in the analysis of optical and UV spectra of active galaxies. She is well versed in the methodology and software for decomposing spectra, fitting the continuum, and measuring the properties of the emission lines. She also has extensive expertise in the physics of active galaxies and models for their emission lines as well as expertise in multi-phase outflows from active galactic nuclei and their hosts.
J. Walsh has a great deal of expertise on kinematics and dynamics of the gas in the nuclei of AGNs in general and LINERs in particular. She is also an expert spectroscopist and the lead author of one of the primary papers that motivate this proposal (Walsh et al. et al. 2008, AJ, 136, 1677). In that work she carried out the same analysis of STIS/G750M spectra that we propose to undertake in this project.Supermassive Black Holes and Active GalaxiesGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYLINERNUCLEUSSEYFERTSPIRALThis object was generated by the target selector and retrieved from the SIMBAD database.
Coordinates taken from archival HST observation of object, program 8684.J2000J2000GALAXYELLIPTICALLINERNUCLEUSRADIO GALAXYYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from HST program 7124NGC-4374J2000J2000GALAXYELLIPTICALLINERNUCLEUSYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from HST program 8472NGC-4552J2000J2000GALAXYDUST LANELINERNUCLEUSSPIRALYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from HST program 7354NGC-4594J2000J2000GALAXYLINERNUCLEUSRINGSPIRALYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from HST program 8591NGC-4736J2000J2000GALAXYLINERNUCLEUSSPIRALYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from HST program 7357.J2000J2000GALAXYELLIPTICALLINERNUCLEUSYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
Coordinates taken from program 9107.J2000J2000GALAXYDISKDUST LANELINERNUCLEUSYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYLINERNUCLEUSSPIRALYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750M6581STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG430L4300POS-TARGDITHER0.15LINEfalsefalse390.0STIS-ALONG-SLIT1falseThe scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC1097 with STIS+G750M+52x0.2E1.
Need slit PA=39.1 (+/- 3) deg to match an archival G430L observation from program 8684. Hence we calculate ORIENT = 81.1 to 87.1 and 261.1 to 267.1 (180 deg off).
Using same target coordinates and acquisition method as program 8684, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2 arcsec slit)
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.164379994700081.10000000000002(Tic-Visit
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)true10Duplicating the acquisition method from program 8684.Hst Same orient constraint links visits (02 03 15 18 19)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M84 (a.k.a. NGC4274) with STIS+GG430L+52x0.2E1.
Need slip PA=104.0 (+/- 3) deg to match archival G750M observation from program 7124. Hence we calculate ORIENT = 146.0 to 152.0 and 326.0 to 332.0 (180 deg off)
Using same target coordinates and acquisition method as program 7124, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2" slit). But note that after the target acquisition we need an offset of POS-TARG +0.1, 0 (i.e., 0.1" offset along +X, perpendicular to slit) to match the slit position of that program.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1650542805000148.0(Tic-Visit
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)true32we are duplicating the acquisition method (including exposurte time) from program 8684.Hst Same orient constraint links visits (02 03 15 18 19)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M84 (a.k.a. NGC4274) with STIS+GG430L+52x0.2E1.
As in the previous visit, we need sli PA=104.0 (+/- 3) deg to match archival G750M observation from program 7124. Hence we calculate ORIENT = 146.0 to 152.0 and 326.0 to 332.0 (180 deg off).
Using same target coordinates and acquisition method as program 7124, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2" slit). But note that after the target acquisition we need an offset of POS-TARG +0.1, 0 (i.e., 0.1" offset along +X, perpendicular to slit) to match the slit position of that program.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1650205600000148.0(Tic-Visit
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)true20we are duplicating the acquisition method (including exposurte time) from program 8684.The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M89 (a.ka. NGC4552) with STIS+G430L+52x0.1E1.
Need slit PA=78.0 (+/- 3) deg to match archival G750M observation from program 8472. Hence we calculate ORIENT = 120.0 to 126.0 and 300.0 to 306.0 (180 deg off)
Using same target coordinates and acquisition method as program 8472: ACQTYPE=DIFFUSE and CHECKBOX=3, followed by ACK/PEAK since we are using the 0.1" slit.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1650634286000120.0(Tic-Visit
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)true30we are duplicating the acquisition method (including exposurte time) from program 8684.we are duplicating the acquisition method (including exposurte time) from program 8684.The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M104 (a.k.a. NGC4594) with STIS+G750M+52x0.2E1. and STIS+G430L+52x0.2E1.
Using same target coordinates as program 7354.
Any ORIENT is fine for this visit as all exposures are done at the same ORIENT.
Using ACQTYPE=POINT, but no ACK/PEAK since we are using the 0.2" slit.
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:si-vis-utilization 2532
:al-overhead-at-end 75
:internal-dur-at-end 360
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true20we are duplicating the acquisition method (including exposurte time) from program 8684.The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M94 (a.k.a. NGC4736) with STIS+G430L+52x0.2E1.
Using same target coordinates and acquisition method as program 8591: ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1650983148000134.94968(Tic-Visit
:proposal-id 16772
:visit-id "06"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:23.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221280
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "06"
:obset-id "06"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "06"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2532
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "06"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "06"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true30we are duplicating the acquisition method (including exposurte time) from program 8684.The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M94(a.k.a. NGC4736) with STIS+G750M+52x0.2E1.
Need same ORTIENT as previous visit so that the slit will cover the same portion of the galaxy and we can then combine the G430L and G750M spectra
Using same target coordinates and acquisition method as program 8591: ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1652177461000134.94968(Tic-Visit
:proposal-id 16772
:visit-id "07"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:25.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "07"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "07"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true20we are duplicating the acquisition method (including exposurte time) from program 8684.The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC3507 STIS+G430L+52x0.2E1 followed by STIS+G750M+52x0.2E1
Any ORIENT is fine for this visit as long as all exposures are done at the same ORIENT.
Using the same coordinates and acquisition method as a previous STIS observation from program 7357. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2" slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1646837989000164.69758538074637(Tic-Visit
:proposal-id 16772
:visit-id "08"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:28.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 239680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "08"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2643
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "08"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "08"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2643
:al-overhead-at-end 75
:internal-dur-at-end 439
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)true30Hst Same orient constraint links visits (09 10 16 17)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.8. NGC3607-G430L
NGC3607+G430L+52x0.2E1
Any ORIENT is fine for this visit but the next visit with G750M will have to match the same ORIENT (or 180 deg off).
Using the same coordinates and almost same acquisition method as a previous STIS observation from program 9107. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1651394202000114.09692000000001(Tic-Visit
:proposal-id 16772
:visit-id "09"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:31.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221280
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "09"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2642
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "09"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "09"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)true30Hst Same orient constraint links visits (09 10 16 17)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC3607+G750M+52x0.2E1
Need to match the same ORIENT as previous visit of same object with G430L (or 180 deg off).
Using the same coordinates and almost same acquisition method as a previous STIS observation from program 9107. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1650719784000114.09692000000001(Tic-Visit
:proposal-id 16772
:visit-id "10"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:33.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "10"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2643
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "10"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)true20The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC4438+G430L+52x0.2E1
The coordinates are the of the nuclear radio core (detected with the VLA by Hota et al. 2007, MNRAS, 380, 1009). There is also a strong H-alpha source (resolved with WFC3 at FWHM 0.3 arcsec; see Kenney & Yale 2002, ApJ, 567, 865)
Any ORIENT is fine for this visit but the next visit with G750M will have to match the same ORIENT (or 180 deg off).
Using diffuse acquisition since we do not know if there is a prominent optical point source in this galaxy ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID). No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.165501827200096.5(Tic-Visit
:proposal-id 16772
:visit-id "11"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:35.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221280
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "11"
:obset-id "11"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "11"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2633
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "11"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2635
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "11"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2635
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)true30The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC4438+G750M+52x0.2E1
Need to match the same ORIENT as previous visit of same object with G430L (or 180 deg off).
Using the same coordinates acquisition method as the previous visit of the same object. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.165493826500096.5(Tic-Visit
:proposal-id 16772
:visit-id "12"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:38.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "12"
:obset-id "12"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "12"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2634
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "12"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2635
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3015
:pcs-gap 0
)true20The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC4457+G430L+52x0.2E1
The coordinates of the galaxy nucleus from SDSS DR13. They agree to 0.2" with 2MASS coordinates (reported on NED). They also agree to 0.04" with the coordinates of the nuclear X-ray source detected by Chandra (reported in Liu 2011, ApJS, 192, 10).
Any ORIENT is fine for this visit but the next visit with G750M will have to match the same ORIENT (or 180 deg off).
Using diffuse acquisition since we do not know if there is a prominent optical point source in this galaxy ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID). No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1656424123000114.84204(Tic-Visit
:proposal-id 16772
:visit-id "13"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:40.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221280
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "13"
:obset-id "13"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "13"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2625
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3005
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "13"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2623
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3005
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "13"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2623
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3005
:pcs-gap 0
)true30The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC4457+G750M+52x0.2E1
Need to match the same ORIENT as previous visit of same object with G430L (or 180 deg off).
Using the same coordinates acquisition method as the previous visit of the same object. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1655475844000114.84204(Tic-Visit
:proposal-id 16772
:visit-id "14"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:45.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "14"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2623
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3005
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "14"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2623
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3005
:pcs-gap 0
)true20Hst Same orient constraint links visits (02 03 15 18 19)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M84 (a.k.a. NGC4274) with STIS+GG430L+52x0.2E1.
Need slip PA=104.0 (+/- 3) deg to match archival G750M observation from program 7124. Hence we calculate ORIENT = 146.0 to 152.0 and 326.0 to 332.0 (180 deg off)
Using same target coordinates and acquisition method as program 7124, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2" slit). But note that after the target acquisition we need an offset of POS-TARG +0.1, 0 (i.e., 0.1" offset along +X, perpendicular to slit) to match the slit position of that program.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1680091026000148.0(Tic-Visit
:proposal-id 16772
:visit-id "15"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:48.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221248
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "15"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2529
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "15"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "15"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true30we are duplicating the acquisition method (including exposurte time) from program 8684.Hst Same orient constraint links visits (02 03 15 18 19)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M84 (a.k.a. NGC4274) with STIS+GG430L+52x0.2E1.
HOPR copy of visit 15
Need slip PA=104.0 (+/- 3) deg to match archival G750M observation from program 7124. Hence we calculate ORIENT = 146.0 to 152.0 and 326.0 to 332.0 (180 deg off)
Using same target coordinates and acquisition method as program 7124, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2" slit). But note that after the target acquisition we need an offset of POS-TARG +0.1, 0 (i.e., 0.1" offset along +X, perpendicular to slit) to match the slit position of that program.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1712426017000148.0(Tic-Visit
:proposal-id 16772
:visit-id "18"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:51.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 221248
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "18"
:obset-id "18"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "18"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2529
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "18"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "18"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2533
:al-overhead-at-end 0
:internal-dur-at-end 419
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true30we are duplicating the acquisition method (including exposurte time) from program 8684.Hst Same orient constraint links visits (09 10 16 17)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.8. NGC3607-G430L
NGC3607+G430L+52x0.2E1
Any ORIENT is fine for this visit but the next visit with G750M will have to match the same ORIENT (or 180 deg off).
Using the same coordinates and almost same acquisition method as a previous STIS observation from program 9107. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1683286877000114.09692000000001(Tic-Visit
:proposal-id 16772
:visit-id "16"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:53.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "16"
:obset-id "16"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "16"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2642
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "16"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)true20Hst Same orient constraint links visits (09 10 16 17)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.NGC3607+G750M+52x0.2E1
Need to match the same ORIENT as previous visit of same object with G430L (or 180 deg off).
Using the same coordinates and almost same acquisition method as a previous STIS observation from program 9107. ACQTYPE=DIFFUSE (CHECKBOX=3, FLUX-CENTROID).
No ACK/PEAK needed since we are using the 0.2 arcsec slit
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.1683201287000114.09692000000001(Tic-Visit
:proposal-id 16772
:visit-id "17"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 16:52:56.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 147680
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "17"
:obset-id "17"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "17"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2643
:al-overhead-at-end 0
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16772
:visit-id "17"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2641
:al-overhead-at-end 0
:internal-dur-at-end 340
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3023
:pcs-gap 0
)true20Hst Same orient constraint links visits (02 03 15 18 19)The scheduling data was generated by CASM 32.1.1.CASM was run in Phase II mode.M84 (a.k.a. NGC4274) with STIS+GG430L+52x0.2E1.
HOPR 92866: copy of first orbit of visit 18
Need slip PA=104.0 (+/- 3) deg to match archival G750M observation from program 7124. Hence we calculate ORIENT = 146.0 to 152.0 and 326.0 to 332.0 (180 deg off)
Using same target coordinates and acquisition method as program 7124, since galaxy is known to have a point source at the nucleus. ACQTYPE=POINT without ACQ/PEAK (since we are using 0.2" slit). But note that after the target acquisition we need an offset of POS-TARG +0.1, 0 (i.e., 0.1" offset along +X, perpendicular to slit) to match the slit position of that program.
Using 3-point dither pattern along slit and setting CR-SPLIT=NO in the individual sub-exposures.(Tic-Visit
:proposal-id 16772
:visit-id "19"
:proposal-version -1
:trans-version "20240604"
:date "12-Aug-2024 22:31:21.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 74032
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16772
:visit-id "19"
:obset-id "19"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16772
:visit-id "19"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2532
:al-overhead-at-end 0
:internal-dur-at-end 380
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2913
:pcs-gap 0
)true10we are duplicating the acquisition method (including exposurte time) from program 8684.