This investigator's institution has no country in the STScI database.0Assigned ID: 3156
----- Attempting Submission 1 (Fri Mar 25 08:07:01 GMT 2022) -----
HST Phase I Proposal 3156 successfully submitted.
Receipt: # 3156-1The country of Co-I Girish Kulkarni's institution is somehow missing, but is listed in the MyST profile.0----- Attempting Submission 1 (Wed Jul 06 16:53:54 GMT 2022) -----The First Dedicated Spectroscopic Extreme UV Survey of Low-Luminosity Broad-Line Active Galactic NucleiCharacterizing the peak of the spectral energy distribution of unobscured broad-line active galactic nuclei (BLAGN) in the extreme UV is key to understand accretion onto supermassive black holes, and to calculate the budget of ionizing photons produced by BLAGN over cosmic time. While theory predicts that the peak and shape of this so-called Big Blue Bump should change with black hole mass and luminosity, existing UV composite spectra of BLAGN are either based on simplistic aggregates of archival data or just on luminous quasars. We propose the first dedicated spectroscopic survey to study the Big Blue Bump of low-luminosity BLAGN with HST/COS. Limited archival data on five mostly serendipitously observed objects reveal typical BLAGN UV continua, one of which is truncated by Lyman continuum absorption of neutral gas in the host environment. This may support limited indications from photometry that the Lyman continuum escape fraction of faint BLAGN is no longer unity. Leveraging a uniform SDSS sample of 20 low-redshift (0.27<z<0.40) low-luminosity (-21<M_1450<-20.6) BLAGN we request 20 orbits of HST/COS to (1) Characterize their average extreme UV spectrum, (2) Test predictions from AGN accretion disk models that the peak of the Big Blue Bump changes significantly within our sample that spans a range in black hole mass and Eddington ratio, and (3) Determine the average Lyman continuum escape fraction of low-luminosity BLAGN. Finding significant Lyman continuum emission in these local analogs of z>4 BLAGN discovered in recent surveys would demand an increased contribution of BLAGN to the UV background, and possibly to reionization.We will obtain COS FUV G140L spectra of 20 low-luminosity broad-line active galactic nuclei at z~0.3 to measure their Lyman continuum properties. All targets have sufficiently accurate GALEX FUV and NUV magnitudes, and are safe to observe with COS. Their SDSS coordinates are accurate enough for efficient acquisition with ACQ/IMAGE. Due to our restriction to compact SDSS sources we expect that the NUV image is dominated by the central point source. To account for minor host galaxy light we aim at a point-source S/N= 40 instead of the minimum of 20, yielding acquisition exposure times between 25 and 75 seconds. The COS G140L grating offers the required broad spectral coverage, while resolving the Lyman break region and the broad UV emission lines. We will employ the 800A setting to contiguously cover the Lyman continuum of our targets at all FP-POS offsets. With realistic COS mock spectra (S/N=8-10 per Angstrom at the Lyman limit in the AGN rest frame obtained in a 2000 seconds spectroscopic exposure) we verified our ability to discriminate between Lyman continuum escape fractions of unity and <0.7 for individual AGN. Stacking the 20 spectra we recover the mean AGN UV spectrum to better than 5-10% in the Lyman continuum, while probing ~10% deviations from unit escape fraction for the low-luminosity AGN population. Spectra will be recorded in TIME-TAG mode with concurrent wavelength calibration (TAGFLASH), and at all FP-POS offsets to correct for COS detector blemishes. Time intervals spent in the Earth's shadow will be used to correct for geocoronal OI and NI emission. Given our faint sources, airglow will dominate the COS count rates. However, even at the high airglow conditions conservatively assumed in our spectroscopic ETC calculations, the buffer time is longer than the exposure time. We have set all buffer times to 4800 seconds, filling the overhead between FP-POS moves. All exposure times have been adjusted to use the full visibility period in each orbit.
Reduced gyro operations will not affect our program, because our visits have no orientation constraints. APT indicates a sufficient number of scheduling windows for our one-orbit visits.Our team combines the observational and theoretical expertise to perform the proposed research project to conduct the first dedicated spectroscopic extreme UV survey of low-luminosity broad-line active galactic nuclei with HST/COS.
The PI, Dr. Gabor Worseck, is an expert in observational studies to constrain the UV background and quasar-driven helium reionization. He is a renowned expert in the reduction and analysis of HST/COS data in the low-count Poisson regime with custom software that correctly estimates dark current and scattered light in the COS aperture (e.g. Worseck et al. 2016, ApJ, 825, 144; Worseck et al. 2019, ApJ, 875, 111). His custom pipeline has recently been published in Makan et al. (2021, ApJ, 912, 38), and is used in HST/COS studies of Lyman continuum emission from star-forming galaxies (e.g. Izotov et al. 2018, MNRAS, 478, 4851; Flury et al. 2022, ApJS, accepted, arXiv:2201.11716). He designed the proposed survey and selected the targets.
Dr. Elisabeta Lusso has led the first dedicated study of the Big Blue Bump of luminous quasars (Lusso et al. 2015, MNRAS, 449, 4204). There we introduced the stacking technique and the correction of intergalactic absorption that will also be employed in the proposed analysis. Follow-up investigations for the proposed sample could include studies on the UV-X-ray correlation (e.g. Lusso & Risaliti 2016, ApJ, 819, 154).
Dr. Girish Kulkarni has broad expertise in numerical simulations of reionization (Kulkarni et al. 2019, MNRAS, 485, L24) and has led a large meta-analysis of the BLAGN luminosity function and their contribution to the UV background (Kulkarni et al. 2019, MNRAS, 488, 1035). While this work has provide the first consistent determinations of the BLAGN emissivity from the highly covariant luminosity function, the assumption of a unity Lyman continuum escape fraction is to be tested with the observations proposed here.
Dr. Frederick Davies is an expert in modeling the UV background (e.g. Davies & Furlanetto 2016, MNRAS, 460, 1328). He will supply radiative transfer models of the enhanced UV radiation field around the faint BLAGN (e.g. Davies et al. 2020, MNRAS, 493, 1330). Unlike luminous quasars, the faint BLAGN studied here may not be able to ionize dense gas in their surroundings, giving rise to proximate Lyman limit breaks.
Dr. Jonathan Stern has worked on the properties of low-redshift BLAGN (e.g. Stern & Laor 2013, MNRAS, 431, 836), on the physics of the circumgalactic medium (e.g. Stern et al. 2016, ApJ, 830, 87), and BLAGN feedback mechanisms (e.g. Stern et al. 2016, ApJ, 819, 130).
Professors Gordon Richards, Joseph Hennawi, J. Xavier Prochaska provide senior advice on data analysis, modeling, and interpretation of the results. They are renowned experts in all aspects of this project (e.g. Prochaska et al. 2010, ApJ, 718, 392; Richards et al. 2011, AJ, 141, 167; Krawczyk et al. 2013, ApJS, 206, 4; Prochaska et al. 2013, ApJ, 776, 136; Lau et al. 2016, ApJS, 226, 25; Coatman et al. 2017, MNRAS, 465, 2120; Coatman et al. 2019, MNRAS, 486, 5335).Supermassive Black Holes and Active Galaxies6falsefalsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.19+/-0.22 NUV=19.97+/-0.12GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.43+/-0.30 NUV=20.53+/-0.14GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.01+/-0.25 NUV=20.66+/-0.06GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=19.16+/-0.09 NUV=19.71+/-0.01GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.41+/-0.20 NUV=20.24+/-0.14GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.87+/-0.30 NUV=20.50+/-0.18GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.14+/-0.29 NUV=20.52+/-0.18GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.01+/-0.18 NUV=19.52+/-0.09GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.09+/-0.19 NUV=19.79+/-0.11GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=19.27+/-0.10 NUV=19.45+/-0.02GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=19.72+/-0.15 NUV=19.73+/-0.08GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.40+/-0.30 NUV=20.23+/-0.12GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=19.98+/-0.13 NUV=19.59+/-0.09GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.28+/-0.21 NUV=20.35+/-0.17GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.07+/-0.35 NUV=20.31+/-0.10GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.28+/-0.07 NUV=20.58+/-0.04GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.35+/-0.12 NUV=20.67+/-0.06GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.25+/-0.17 NUV=19.97+/-0.12GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=20.86+/-0.08 NUV=20.04+/-0.03GALAXYQSOSEYFERTNOJ2000J2000GALEX FUV=21.35+/-0.29 NUV=20.72+/-0.12COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800COS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1697226117000281.71787064581963(Tic-Visit
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