ACCRETION RATES OF RED QUASARS FROM THE HYDROGEN P<i>β</i>LINE

Kim, Dohyeong; Im, Myungshin; Glikman, Eilat; Woo, Jong-Hak; Urrutia, T.

doi:10.1088/0004-637x/812/1/66

Cited by 38 publications

(68 citation statements)

References 77 publications

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“…Ricci et al (2017a) suggest that the Hot DOGs are underluminous in X-rays owing to their potentially very high Eddington ratios (L/L Edd ∼ 1; Wu et al 2018) and possible saturation of the X-ray-emitting region of the AGN. F2M red quasars have also been shown to have very high Eddington ratios (Urrutia et al 2012;Kim et al 2015), and the same may be the case for the WISEselected sources in this work.…”

Section: Luminosity Relationssupporting

confidence: 77%

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗

Glikman

Lacy

LaMassa

et al. 2018

ApJ

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We present a spectroscopically complete sample of 147 infrared-color-selected active galactic nuclei (AGNs) down to a 22 μm flux limit of 20 mJy over the ∼270 deg 2 of the Sloan Digital Sky Survey Stripe 82 region. Most of these sources are in the QSO luminosity regime (L bol  10 12 L e ) and are found out to z;3. We classify the AGNs into three types, finding 57 blue, unobscured Type-1 (broad-lined) sources; 69 obscured, Type-2 (narrow-lined) sources; and 21 moderately reddened Type-1 sources (broad-lined and E(B − V )>0.25). We study a subset of this sample in X-rays and analyze their obscuration to find that our spectroscopic classifications are in broad agreement with low, moderate, and large amounts of absorption for Type-1, red Type-1, and Type-2 AGNs, respectively. We also investigate how their X-ray luminosities correlate with other known bolometric luminosity indicators such asand infrared luminosity (L 6μm ). While the X-ray correlation with L [O III] is consistent with previous findings, the most infrared-luminous sources appear to deviate from established relations such that they are either underluminous in X-rays or overluminous in the infrared. Finally, we examine the luminosity function evolution of our sample, and by AGN type, in combination with the complementary, infrared-selected, AGN sample of Lacy et al. (2013), spanning over two orders of magnitude in luminosity. We find that the two obscured populations evolve differently, with reddened Type-1 AGNs dominating the obscured AGN fraction (∼30%) for L 5μm >10 45 erg s −1 , while the fraction of Type-2 AGNs with L 5μm <10 45 erg s −1 rises sharply from 40% to 80% of the overall AGN population.

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Section: Luminosity Relationssupporting

confidence: 77%

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗

Glikman

Lacy

LaMassa

et al. 2018

ApJ

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“…In this work, we used 20 red quasars at 0.186 < z < 0.842 that are composed of 16 red quasars (z > 0.5 and L bol > 10 46 erg s −1 ) studied in Kim et al (2015b) and four additional red quasars (z < 0.5 and L bol ∼ 10 46 erg s −1 ). These 20 red quasars are a subsample of ∼80 spectroscopically confirmed red quasars in Glikman et al (2007) and Urrutia et al (2009), which were selected to be red quasars based on their broadband colors (R − K > 4 and J − K > 1.7 mag in Glikman et al 2007; r − K > 5 and J − K > 1.3 mag in Urrutia et al 2009) from radio-detected 2MASS point sources.…”

Section: Sample and Datamentioning

confidence: 99%

“…For 13 of the 20 red quasars, both the optical and NIR spectra are available and the remaining objects have only NIR spectra. The optical spectra of the red quasars come from Glikman et al (2007Glikman et al ( , 2012 while the NIR spectra are from Glikman et al (2007Glikman et al ( , 2012 and Kim et al (2015b). Additionally, new NIR spectra were obtained for two red quasars (0036−0113 and 1307+2338) using the SpeX instrument (Rayner et al 2003) on the NASA Infrared Telescope Facility (IRTF).…”

Section: Sample and Datamentioning

confidence: 99%

“…For the lines with no detection, we set upper limits. For the upper limits of the Hβ line luminosity, we assume the full width at half maximum (FWHM) of typical red quasars of 3000 km s −1 (Kim et al 2015b). Then, the 5-sigma limit of the integrated luminosity density within the wavelength width of the FWHM value is adopted.…”

Section: Sample and Datamentioning

confidence: 99%

“…So far, observational signatures of red quasars tend to support this picture. For example, red quasars have (i) higher BH accretion rates than unobscured type 1 quasars by factors of 4 to 5 (Urrutia et al 2012;Kim et al 2015b), (ii) enhanced star formation activities (Georgakakis et al 2009), (iii) a high fraction of merging features (Urrutia et al 2008;Glikman et al 2015), and (iv) young radio jets (Georgakakis et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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What makes red quasars red?

Kim

2018

A&A

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Red quasars are very red in the optical through near-infrared (NIR) wavelengths, which is possibly due to dust extinction in their host galaxies as expected in a scenario in which red quasars are an intermediate population between merger-driven star-forming galaxies and unobscured type 1 quasars. However, alternative mechanisms also exist to explain their red colors: (i) an intrinsically red continuum; (ii) an unusual high covering factor of the hot dust component, that is, CFHD = LHD∕Lbol, where the LHD is the luminosity from the hot dust component and the Lbol is the bolometric luminosity; and (iii) a moderate viewing angle. In order to investigate why red quasars are red, we studied optical and NIR spectra of 20 red quasars at z ~ 0.3 and 0.7, where the usage of the NIR spectra allowed us to look into red quasar properties in ways that are little affected by dust extinction. The Paschen to Balmer line ratios were derived for 13 red quasars and the values were found to be ~10 times higher than unobscured type 1 quasars, suggesting a heavy dust extinction with AV > 2.5 mag. Furthermore, the Paschen to Balmer line ratios of red quasars are difficult to explain with plausible physical conditions without adopting the concept of the dust extinction. The CFHD of red quasars are similar to, or marginally higher than, those of unobscured type 1 quasars. The Eddington ratios, computed for 19 out of 20 red quasars, are higher than those of unobscured type 1 quasars (by factors of 3−5), and hence the moderate viewing angle scenario is disfavored. Consequently, these results strongly suggest the dust extinction that is connected to an enhanced nuclear activity as the origin of the red color of red quasars, which is consistent with the merger-driven quasar evolution scenario.

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Red Quasars: Estimation of SMBH Spin, Mass, and Accretion Disk Inclination Angle

Piotrovich,

Buliga,

Natsvlishvili

2024

Astron Nachr

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We estimated values of spin, mass, and inclination angle for sample of 42 red quasars. Our estimations show that two objects: F2MS J1113+1244 and F2MS J1434+0935 with the highest Eddington ratios may have geometrically thick disk. Six objects: SDSS J0036‐0113, S82X 0040+0058, S82X 0118+0018, S82X 0303‐0115, FBQS J1227+3214, S82X 2328‐0028 may have “retrograde” rotation. Analysis of estimated spin values shows that red quasar population may contain Seyfert galaxies and NLS1.

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ACCRETION RATES OF RED QUASARS FROM THE HYDROGEN PβLINE

Cited by 38 publications

References 77 publications

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗

What makes red quasars red?

Red Quasars: Estimation of SMBH Spin, Mass, and Accretion Disk Inclination Angle

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ACCRETION RATES OF RED QUASARS FROM THE HYDROGEN PβLINE

Cited by 38 publications

References 77 publications

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82∗

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82∗

What makes red quasars red?

Red Quasars: Estimation of SMBH Spin, Mass, and Accretion Disk Inclination Angle

Contact Info

Product

Resources

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Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗

Luminous WISE-selected Obscured, Unobscured, and Red Quasars in Stripe 82^∗