For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.Version #4 (prime-prime), tweaked the text further...1827023280Assigned ID: 6331
----- Attempting Submission 1 (Thu Apr 10 00:38:53 GMT 2025) -----
HST Phase I Proposal 6331 successfully submitted.
Receipt: # 6331-1
----- Attempting Submission 2 (Thu Apr 10 00:51:21 GMT 2025) -----
HST Phase I Proposal 6331 successfully submitted.
Receipt: # 6331-2
----- Attempting Submission 3 (Thu Apr 10 02:02:08 GMT 2025) -----
HST Phase I Proposal 6331 successfully submitted.
Receipt: # 6331-3
----- Attempting Submission 4 (Thu Apr 10 20:07:37 GMT 2025) -----
HST Phase I Proposal 6331 successfully submitted.
Receipt: # 6331-4
----- Attempting Submission 5 (Thu Apr 10 21:28:10 GMT 2025) -----
HST Phase I Proposal 6331 successfully submitted.
Receipt: # 6331-5
----- Attempting Submission 6 (Thu Apr 10 23:30:53 GMT 2025) -----The proposed lifetime usage of LP5, LP7, and LP10 is well below the 2% cap, as stated in the Description of the Observations.For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.Version #2. Same as version #1 except the exposure times for visit #20 (NGC 4395 G160M) were reduced to 850 seconds following the STScI staff recommendation to help with the GS.
Version #3. Following the STScI recommendations, all G160M observations for a given object now use all four FP-POS settings. In two cases (visits 6 and 23), this meant splitting one of the orbits into two observations with different FP-POS settings (and four observations in the case of the one-orbit visit #20 on NGC 4395 with FP-POS = ALL).-984472361----- Attempting Submission 1 (Tue Jul 29 15:30:56 GMT 2025) -----
HST Phase II Proposal 18134 successfully submitted.
Receipt: # 18134-1
----- Attempting Submission 2 (Wed Jul 30 13:57:59 GMT 2025) -----
----- Attempting Submission 3 (Mon Nov 17 18:32:09 GMT 2025) -----Version #1. All warnings are about inefficient use of FP-POS settings but the emphasis here is on having long uninterrupted exposures of these faint sources for maximum S/N where the noise is from the detector.
Version #3. Following the STScI recommendations, all G160M observations for a given object now use all four FP-POS settings. In two cases (visits 6 and 23), this meant splitting one of the orbits into two observations with different FP-POS settings (and four observations in the case of the one-orbit visit #20 on NGC 4395 with FP-POS = ALL).A Far-Ultraviolet Spectroscopic Survey of AGN Dwarf GalaxiesThe far-ultraviolet (FUV) band below 2000 A is rich in spectroscopic diagnostics of the massive star populations, active galactic nuclei, and neutral and ionized gas phases of the ISM. The recent launch of JWST has ushered in a new era of extragalactic astronomy where these diagnostic tools have been used extensively to study galaxies at the epoch of reionization, down to stellar masses below that of the LMC. An unexpectedly large fraction of these galaxies appear to host fast-accreting massive black holes (BHs), but the exact role played by the AGN in powering the emission lines and driving outflows is still highly uncertain due in part to our incomplete understanding of AGN physics in dwarf galaxies. CLASSY has provided a comprehensive FUV spectral database of nearby star-forming galaxies, which has shed light on the ISM conditions and processes associated with massive stars in dwarf galaxies, but AGN dwarf galaxies have largely been excluded. To address this weakness, we propose a sensitive high-resolution FUV spectroscopic study of 8 nearby sub-LMC dwarf galaxies with AGN that span a broad range of BH masses, Eddington ratios, and host properties. The COS spectra will allow us to explore, for the first time in dwarf galaxies: (1) the dependence of FUV emission line diagnostics on AGN properties, (2) the FUV BLR properties and their use as BH mass indicators, and (3) the rate of incidence and properties of AGN-driven outflows. The resulting data products will serve as local benchmarks to help the community interpret the rest-frame FUV spectra of high-z AGN obtained with JWST and upcoming ELTs. Given the legacy value of these data, the proprietary period is shortened.We observe the central AGN for all 8 dwarf galaxies in our sample with COS G130M and G160M, unless high-S/N spectra already exist in the archives. We also observe the three FUV brightest sources with G185M. The RA and DEC coordinates of these objects are in the ICRS reference frame; they have been verified using the finding chart generated by the Target Confirmation tool of APT. For each visit, we first use ACQ/IMAGE to obtain a NUV image of the field and center the aperture on the intensity peak making use of MIRRORA (except for bright NGC 4395, where we use MIRRORB). The exposure time of 60 seconds for ACQ/IMAGE is generous and typically results in S/N of ~50.
For the G130M (G160M) observations, we request the cenwave = 1291 (1577, 1600, or 1611) A setting with both segments A and B to try to capture redshifted Ly-alpha, N V 1238, 1243, S IV 1394, 1403, C IV 1548, 1550, He II 1640, and possibly weaker lines. For the G185M observations, we use cenwave = 1817, 1850, or 1890 to capture redshifted C III] 1906, 1908, depending on the redshift of each source. Following the STScI recommendations, the observations are split into visits of 3 orbits or less, each consisting of long exposures with FP-POS = 3 or 4 (1, 2, 3, or 4 if using G160M) to reduce the fixed pattern noise. This observing strategy minimizes the overhead and maximize the on-target exposure time, and thus S/N. For NGC 4395, the one-orbit visit is split into four segments of equal lengths with different FP-POS. All of the observations are done in TIME-TAG mode. This temporal sampling will allow us to exclude poor quality data and get improved thermal correction and background removal. For simplicity and to guard against the (unlikely) possibility that our targets are more than ~50% brighter than expected, we generally set buffer-time = exposure-time. In observations where we split the G160M orbits into two segments to get all four FP-POS, we set buffer-time = exposure-time - 110 sec (option #5 in Chap 5.4).
According to the Bright Object Tool (BOT), there are no bright sources near our targets that could cause a problem for COS.Prof. Sylvain Veilleux (U. Maryland) has 30+ years of experience studying starbursts and AGN, near and far, with ground- and space-based facilities including HST. In recent years, he has been the P.I. of several COS programs, focusing on the strong outflows and gaseous environments of low-redshift PG quasars and ULIRGs as well as dwarf galaxies. Dr. Weizhe Liu (U. Arizona) developed his own software to characterize the FUV emission and absorption line profiles in COS spectra and recently published a first-author paper on an analysis of COS G160M spectra in three AGN dwarf galaxies, as part of his PhD thesis under the supervision of PI Veilleux at Maryland. Prof. Todd Tripp is one of the leading experts on the reduction and analysis of COS data. He has led three large HST programs (PID #9184,11741,13846), which have produced 70+ refereed papers, including works from other groups that have analyzed the acquired data with assorted (and usually novel) approaches. Prof. Frederick Hamann has made significant contributions to the field of quasar outflows, especially through optical and UV spectroscopy. He has led a paper on the discovery of an exceptional outflow in PG 1411+442 with COS data (PID #12569). Prof. David Rupke is an expert researcher who has used multiwavelength ground-based and space-based data to study galactic outflows. He has carried out an HST/STIS NUV spectroscopy observation of the galactic wind in a local ULIRG (PID #14184).GalaxiesSupermassive Black Holes and Active Galaxies3falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALEX: m_fuv = 19.29, m_nuv = 19.30GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX: m_fuv = 19.01, m_nuv = 18.81GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALEX: m_fuv = 20.01, m_nuv = 19.47GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALEX: m_fuv = 20.47, m_nuv = 19.75GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX: m_fuv = 19.94, m_nuv = 19.58GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALEX: m_fuv = 19.82, m_nuv = 19.43GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALEX: m_fuv = 17.4, m_nuv = 16.7 (variable)GALAXYNUCLEUSNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALEX: m_fuv = 19.04, m_nuv = 18.73COS/FUVSpectroscopicNoNoG130M1327COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG160M1533COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1327COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG160M1533COS/NUVImagingNoNoMIRRORACOS/NUVSpectroscopicNoNoG185M1890COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1327COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1291COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1327COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1327COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG160M1533COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1291COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG160M1600COS/NUVImagingNoNoMIRRORACOS/NUVSpectroscopicNoNoG185M1817COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG130M1309COS/NUVImagingNoNoMIRRORACOS/FUVSpectroscopicNoNoG160M1623COS/NUVImagingNoNoMIRRORACOS/NUVSpectroscopicNoNoG185M1850COS/NUVImagingNoNoMIRRORAThe scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.(Tic-Visit
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