0
Assigned ID: 770
----- Attempting Submission 1 (Fri Mar 06 20:58:43 GMT 2020) -----
HST Phase I Proposal 770 successfully submitted.
Receipt: # 770-1
----- Attempting Submission 2 (Fri Mar 06 21:56:26 GMT 2020) -----
HST Phase I Proposal 770 successfully submitted.
Receipt: # 770-2
The number of orbits used exceeds the number allocated
visit 16 copied to 33 HOPR repeat
-2113067839
----- Attempting Submission 1 (Tue Jun 23 11:38:15 GMT 2020) -----
----- Attempting Submission 2 (Mon Aug 17 14:38:13 GMT 2020) -----
The First Measurement of the Distribution of Quasar Lifetimes with the HeII Proximity Effect
The duration of quasar (QSO) accretion episodes is a key quantity for distinguishing between models for the formation and growth of supermassive black holes, QSO evolution, and the potential feedback effects on their host galaxies. However, this critical timescale, often referred to as the QSO lifetime, is still uncertain by orders of magnitude t_Q~10^4-10^9 yr. The intense UV radiation from a QSO dramatically alters the ionization state of its surrounding intergalactic medium (IGM), which is observable as enhanced Lyman-alpha transmission toward the QSO in its so-called proximity zone. HST/COS spectra of far-UV bright QSOs probing the HeII Lyman-alpha forest provide a unique opportunity to make precise lifetime measurements for individual QSOs. Indeed, the size of the HeII proximity zone depends sensitively on the QSO lifetime for t_Q<30 Myr, comparable to the e-folding timescale for SMBH growth t_S=45 Myr. We have compared the sizes of HeII proximity zones to theoretical models generated by post-processing cosmological hydrodynamical simulations with 1D radiative transfer, which allows us to measure individual QSO lifetimes to 0.2 dex precision. An analysis of 24 archival HST/COS spectra has revealed a surprisingly broad distribution of lifetimes ranging from <1 to >30 Myr. These results point to complex QSO light curves that exhibit structure on a wide range of timescales. By leveraging a new sample of FUV-bright QSOs selected from GALEX, SDSS, PanSTARRS and WISE, we request 32 orbits of HST/COS to double the number of QSOs to which we can apply this exciting new technique, which will allow us to make the first measurement of the distribution of QSO lifetimes.
We will obtain COS FUV G140L spectra of 32 FUV-bright quasars at 2.7<z<3.2 to measure their HeII Lyman alpha proximity zone sizes. All targets have sufficiently accurate GALEX FUV and NUV magnitudes, and are safe to observe with COS. Their SDSS and Pan-STARRS coordinates are accurate enough for efficient acquisition with ACQ/IMAGE. The NUV imaging target acquisition exposure times to reach the recommended S/N=20 range from 20 to 90 seconds depending on the target NUV magnitude.
The COS G140L grating is optimal for efficient verification of the FUV flux and the measurement of the proximity zones. We will employ the 800A setting to contiguously cover the z>2.5 HeII Lyman alpha absorption, the HeII proximity zone, and the quasar continuum. With realistic COS mock spectra we verified our ability to measure the HeII proximity zone size of every target in a ~2000 seconds spectroscopic exposure, corresponding to a one-orbit visit per target (Fig. 8 in the proposal). 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 ETC calculations, the buffer time is longer than the exposure time. 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 determine the distribution of QSO lifetimes via the HeII proximity effect with HST/COS.
The PI, Dr. Gabor Worseck, is an expert in observational studies to constrain the reionization epochs of hydrogen and helium with quasar spectroscopy. 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). He has led five related HST/COS programs in Cycles 17-25 that have resulted in 8 published papers so far. He has led the ground-based survey for FUV-bright QSOs from which many ouf our targets are drawn.
Dr. Ilya Khrykin has developed the Bayesian method to determine QSO lifetimes from the HeII proximity effect, which has been applied to 7 QSOs in Khrykin et al. (2019, MNRAS, 484, 3897). In our proposal we apply this method to more archival data. He is supplying new one-dimensional radiative transfer simulations of HeII QSO proximity zones for comparison with the HST/COS data run with his code (Khrykin et al. 2016, ApJ, 824, 133).
Dr. Frederick B. Davies is an expert in semi-analytic modeling of the fluctuating HeII-ionizing background (Davies & Furlanetto 2014, MNRAS, 437, 1141; Davies et al. 2017, MNRAS, 465, 2886), and the proximity effect (Davies et al. 2020, MNRAS, 493, 1330).
Professors Joseph F. Hennawi and J. Xavier Prochaska provide senior advice on data analysis, modeling, and interpretation of the results. They have provided, and will continue to provide, access to the Keck telescopes to perform additional follow-up observations not applied for in this proposal, i.e. to obtain high-resolution optical spectra of the coeval HI absorption along the sightlines, and to search for foreground QSOs near HeII sightlines to reveal the transverse proximity effect of QSOs.
Dr. Tobias Schmidt has been leading the investigations of the transverse proximity effect near archival HeII sightlines to constrain their lifetime and anisotropy (Schmidt et al. 2017, ApJ, 847, 81; Schmidt et al. 2018, ApJ, 861, 122). We plan to extend this analysis to the new HeII sightlines proposed here.
Supermassive Black Holes and Active Galaxies
Intergalactic Medium and the Circumgalactic Medium
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