C iv black hole mass measurements with the Australian Dark Energy Survey (OzDES)

Hoormann, J. K.; Martini, Paul; Davis, Tamara M.; King, A.; Lidman, C.; Mudd, D.; Sharp, Robert; Sommer, N. E.; Tucker, B.; Yu, Zhifeng; Allam, S.; Asorey, J.; Ávila, S.; Banerji, M.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Calcino, Josh; Rosell, A. Carnero; Carollo, D.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Childress, M.; Vicente, J. De; Desai, S.; Diehl, H. T.; Doel, P.; Flaugher, B.; Fosalba, P.; Frieman, Joshua A.; García-Bellido, J.; Gerdes, D. W.; Gruen, David; Gutiérrez, G.; Hartley, W. G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hoyle, B.; James, D. J.; Krause, E.; Kuêhn, K.; Kuropatkin, N.; Lewis, Geraint F.; Lima, M.; Macaulay, E.; Maia, M. A. G.; Menanteau, F.; Miller, C. J.; Miquel, R.; Möller, A.; Plazas, A. A.; Romer, A. K.; Roodman, A.; Sánchez, E.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Smith, M.; Smith, Rory; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swann, E.; Swanson, M. E. C.; Tarlè, G.; Uddin, S. A.

doi:10.1093/mnras/stz1539

Cited by 46 publications

(62 citation statements)

References 74 publications

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“…For the Mg II line, we also fit and subtract the iron emission lines using the template from Vestergaard & Wilkes (2001). We measure the monochromatic luminosity using the fluxcalibrated OzDES spectra (Hoormann et al 2019) and calculate R BLR using the R BLR -luminosity relations from Bentz et al where we do not consider the DES calibration errors, while the red circles represent the cases where we add the DES calibration errors following the same process as the quasar light curves. The black dashed line represents the position where c r 2 equals 1.…”

Section: Disk Size-black Hole Mass Relationmentioning

confidence: 99%

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping in the DES Standard-star Fields

Martini

Davis

et al. 2020

ApJS

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Measurements of the physical properties of accretion disks in active galactic nuclei are important for better understanding the growth and evolution of supermassive black holes. We present the accretion disk sizes of 22 quasars from continuum reverberation mapping with data from the Dark Energy Survey (DES) standard-star fields and the supernova C fields. We construct continuum light curves with the griz photometry that span five seasons of DES observations. These data sample the time variability of the quasars with a cadence as short as 1 day, which corresponds to a rest-frame cadence that is a factor of a few higher than most previous work. We derive time lags between bands with both JAVELIN and the interpolated cross-correlation function method and fit for accretion disk sizes using the JAVELIN thin-disk model. These new measurements include disks around black holes with masses as small as ∼10 7 M e , which have equivalent sizes at 2500 Å as small as ∼0.1 lt-day in the rest frame. We find that most objects have accretion disk sizes consistent with the prediction of the standard thin-disk model when we take disk variability into account. We have also simulated the expected yield of accretion disk measurements under various observational scenarios for the Large Synoptic Survey Telescope Deep Drilling Fields. We find that the number of disk measurements would increase significantly if the default cadence is changed from 3 days to 2 days or 1 day.

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Section: Disk Size-black Hole Mass Relationmentioning

confidence: 99%

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping in the DES Standard-star Fields

Martini

Davis

et al. 2020

ApJS

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“…To explain these facts, a physical scenario might be considered in which microlensing can magnify only a part of the broad emission lines (see, e.g., Popović et al 2001b; Abajas et al 2002,2007). The C IV BLR dimensions can be estimated using the luminosity of the C IV line and nearby continuum (at λ1350Å; see, e.g., Kong et al 2006;Kaspi et al 2007;Trevese et al 2014;Lira et al 2018;Hoormann et al 2019). To estimate a continuum at λ 1350 Å that is not amplified, we first calculated the amplification (A) for each component using (see Wambsganss 1998)…”

Section: Spectroscopic Variabilitymentioning

confidence: 99%

Spectroscopy and polarimetry of the gravitationally lensed quasar SDSS J1004+4112 with the 6m SAO RAS telescope

Afanasiev

Moiseev

Smirnova

et al. 2020

A&A

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Context. We present new spectroscopic and polarimetric observations of the gravitational lens SDSS J1004+4112 taken with the 6m telescope of the Special Astrophysical Observatory (SAO, Russia). Aims. In order to explain the variability that is observed only in the blue wing of the C IV emission line, corresponding to image A, we analyze the spectroscopy and polarimetry of the four images of the lensed system. Methods. Spectra of the four images were taken in 2007, 2008, and 2018, and polarization was measured in the period 2014-2017. Additionally, we modeled the microlensing effect in the polarized light, assuming that the source of polarization is the equatorial scattering in the inner part of the torus. Results. We find that a blue enhancement in the CIV line wings affects component A in all three epochs. We also find that the UV continuum of component D was amplified in the period 2007-2008, and that the red wings of CIII] and CIV appear brighter in D than in the other three components. We report significant changes in the polarization parameters of image D, which can be explained by microlensing.Our simulations of microlensing of an equatorial scattering region in the dusty torus can qualitatively explain the observed changes in the polarization degree and angle of image D. We do not detect significant variability in the polarization parameters of the other images (A, B, and C), although the averaged values of the polarization degree and angle are different for the different images.Conclusions. Microlensing of a broad line region model including a compact outflowing component can qualitatively explain the CIV blue wing enhancement (and variation) in component A. However, to confirmed this hypothesis, we need additional spectroscopic observation in future.

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“…At the same time, OzDES has monitored a sample of 771 AGN up to z ∼ 4 with the goal of measuring black hole masses using the time lag between variations in the continuum, measured from the broad-band photometry obtained by DES, and the broad lines, measured from the spectra obtained by OzDES. The first time lags, based on the first four years of data, were published in Hoormann et al (2019).…”

Section: Des and Ozdesmentioning

confidence: 99%

“…OzDES also continued into a sixth year, but was no longer targeting transients. Instead, OzDES continued with its programme to monitor AGN (King et al 2015;Hoormann et al 2019) and to obtain redshifts of galaxies that hosted transients in earlier years. DES continued to target the 10 DES supernova fields during Y6, but with a reduced frequency of about once a month.…”

Section: Ozdes Operations For Y4 Y5 and Y6mentioning

confidence: 99%

“…In the early years, we used the F-stars to derive the transfer functions for the red and blue arms that were then used throughout the survey, and to develop techniques that used the broadband DES photometry to spectrophotometrically calibrate the spectra of AGN used for the OzDES RM project (Hoormann et al 2019).…”

Section: Observing Strategy Calibration and Data Reductionmentioning

confidence: 99%

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OzDES multi-object fibre spectroscopy for the Dark Energy Survey: results and second data release

Lidman

Tucker

Davis

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as rAB = 24 mag, and 375 000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼ 1.2 and the masses of hundreds of black holes out to z ∼ 4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs.

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C iv black hole mass measurements with the Australian Dark Energy Survey (OzDES)

Cited by 46 publications

References 74 publications

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping in the DES Standard-star Fields

Quasar Accretion Disk Sizes from Continuum Reverberation Mapping in the DES Standard-star Fields

Spectroscopy and polarimetry of the gravitationally lensed quasar SDSS J1004+4112 with the 6m SAO RAS telescope

OzDES multi-object fibre spectroscopy for the Dark Energy Survey: results and second data release

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