BAT AGN spectroscopic survey–II. X-ray emission and high-ionization optical emission lines

Berney, Simon; Koss, Michael; Trakhtenbrot, Benny; Ricci, Cláudio; Lamperti, Isabella; Schawinski, Kevin; Baloković, Mislav; Crenshaw, D. M.; Fischer, Travis C.; Gehrels, N.; Harrison, Fiona A.; Hashimoto, Yoshihiro; Ichikawa, Kohei; Mushotzky, R. F.; Oh, Kyuseok; Stern, Daniel; Treister, Ezequiel; Ueda, Yoshihiro; Veilleux, Sylvain; Winter, L. M.

doi:10.1093/mnras/stv2181

Cited by 77 publications

(96 citation statements)

References 56 publications

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“…A separate BASS study found that the physical slit size, telescope sample, or X-ray obscuration level was not a significant contributor to the scatter in emission-line measurements compared to the X-ray emission (Berney et al 2015) for sources with < < z 0.01 0.4, where the size of the slit is typically kiloparsec scales. With some setups we were able to cover the blue [Ne V] l3426, [O II]l3727, and [Ne III] l3968 region (e.g., Figure 20) in addition to the Hβ and Hα regions (e.g., Figure 21).…”

Section: Appendix Amentioning

confidence: 98%

“…In future studies of this sample we will address in detail specific aspects of AGN physics and SMBH growth. Among the many follow-up opportunities, we note our recently published study of correlations between X-ray continuum emission and narrowline emission (e.g., [O III]; Berney et al 2015); a large study of the NIR spectra of over 100 BAT AGNs (Lamperti et al 2017); and a study of trends in accretion rate with merger stage in interacting AGN hosts (M. Koss et al 2017, in preparation). Another study investigates the role of accretion rate in emission-line ratios (Oh et al 2017) and X-ray properties such as Γ , and obscuration (C. Ricci et al 2017, in preparation).…”

Section: Summary Conclusion and Future Workmentioning

confidence: 99%

“…One of the early science results derived from our analysis-a comparison of X-ray-to-optical line emission-was presented in Berney et al (2015). In Section 2, we discuss the parent sample of Swift-BAT-selected AGNs and the different optical telescopes, instrumental setups, and basic reduction procedures used to collect the spectroscopic data set we use.…”

Section: Introductionmentioning

confidence: 99%

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BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics

Koss

Trakhtenbrot

Ricci

et al. 2017

ApJ

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271

308

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We present the first catalog and data release of the Swift-BAT AGN Spectroscopic Survey. We analyze optical spectra of the majority of the detected AGNs (77%, 642/836)based on their 14-195 keV emission in the 70-month Swift-BATall-sky catalog. This includes redshift determination, absorption and emission-line measurements, and black hole mass and accretion rate estimates for the majority of obscured and unobscured AGNs (74%, 473/642), with 340 measured for the first time. With ∼90% of sources at < z 0.2, the survey represents a significant advance in the census of hard X-ray-selected AGNs in the local universe. In this first catalog paper, we describe the spectroscopic observations and data sets, and our initial spectral analysis. The FWHMs of the emission lines show broad agreement with the X-ray obscuration (∼94%), such that Sy 1-1.8 have < N 10 H 21.9 cm −2 , and Seyfert 2 have > N 10 H 21.9 cm −2 . Seyfert 1.9, however, show a range of column densities. Compared to narrow-line AGNs in the SDSS, the X-ray-selected AGNs have a larger fraction of dusty host galaxies ( a b > H H 5), suggesting that these types of AGN are missed in optical surveys. Using the [O III] λ5007/Hβ and [N II] λ6583/Hα emission-line diagnostic, about half of the sources are classified as Seyferts; ∼15% reside in dusty galaxies that lack an Hβ detection, but for which the upper limits on line emission imply either a Seyfert or LINER,~15% are in galaxies with weak or no emission lines despite high-quality spectra, and a few percent each are LINERS, composite galaxies, H II regions, or in known beamed AGNs.

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Section: Appendix Amentioning

confidence: 98%

Section: Summary Conclusion and Future Workmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics

Koss

Trakhtenbrot

Ricci

et al. 2017

ApJ

Self Cite

271

308

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“…found to correlate only weakly with intrinsic hard X-ray luminosity, which is a more direct measure of the instantaneous power of the central engine (Berney et al 2015). Further, it is possible for the [O III] flux to be affected by dust extinction in the host galaxy (e.g., Zakamska et al 2006), and the relationship between L O III [ ] and bolometric luminosity may be complex, depending, for example, on the extent of the emitting narrow-line region (e.g., Hainline et al 2013Hainline et al , 2014bHainline et al , 2016aHusemann et al 2013).…”

Section: Quasar Samplesmentioning

confidence: 99%

Composite Spectral Energy Distributions and Infrared–Optical Colors of Type 1 and Type 2 Quasars

Hickox

Myers

Greene

et al. 2017

ApJ

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We present observed mid-infrared and optical colors and composite spectral energy distributions (SEDs) of type 1 (broad-line) and 2 (narrow-line) quasars selected from Sloan Digital Sky Survey (SDSS) spectroscopy. A significant fraction of powerful quasars are obscured by dust and are difficult to detect in optical photometric or spectroscopic surveys. However, these may be more easily identified on the basis of mid-infrared (MIR) colors and SEDs. Using samples of SDSS type 1 and 2 matched in redshift and [O III] luminosity, we produce composite restframe 0.2-15 μm SEDs based on SDSS, UKIDSS, and Wide-field Infrared Survey Explorer photometry and perform model fits using simple galaxy and quasar SED templates. The SEDs of type 1 and 2 quasars are remarkably similar, with the differences explained primarily by the extinction of the quasar component in the type 2 systems. For both types of quasar, the flux of the active galactic nucleus (AGN) relative to the host galaxy increases with AGN luminosity (L O III [ ] ) and redder observed MIR color, but we find only weak dependencies of the composite SEDs on mechanical jet power as determined through radio luminosity. We conclude that luminous quasars can be effectively selected using simple MIR color criteria similar to those identified previously (W1 W2 0.7; > -Vega), although these criteria miss many heavily obscured objects. Obscured quasars can be further identified based on optical-IR colors (for example, u W3 AB). These results illustrate the power of large statistical studies of obscured quasars selected on the basis of MIR and optical photometry.

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“…The [O III] emission line versus X-ray luminosity relation from Berney et al (2015) is presented in Figure 8, with the shaded region corresponding to the 1σ confidence level from the original study. Overplotted are all the bona fide CTK sources from Table 3.…”

Section: Multiwavelength Indicatorsmentioning

confidence: 99%

IC 3639—A NEW BONA FIDE COMPTON-THICK AGN UNVEILED BY NuSTAR

Boorman

Gandhi

Alexander

et al. 2016

ApJ

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We analyse high-quality NuSTAR observations of the local (z = 0.011) Seyfert 2 active galactic nucleus (AGN) IC 3639, in conjunction with archival Suzaku and Chandra data. This provides the first broadband X-ray spectral analysis of the source, spanning nearly two decades in energy (0.5 -30 keV). Previous X-ray observations of the source below 10 keV indicated strong reflection/obscuration on the basis of a pronounced iron fluorescence line at 6.4 keV. The hard X-ray energy coverage of NuSTAR, together with self-consistent toroidal reprocessing models, enables direct broadband constraints on the obscuring column density of the source. We find the source to be heavily Compton-thick (CTK) with an obscuring column in excess of 3.6 × 10 24 cm −2 , unconstrained at the upper end. We further find an intrinsic 2 -10 keV luminosity of log 10 (L 2 -10 keV [erg s−1 ]) = 43.4 +0.6 −1.1 to 90% confidence, almost 400 times the observed flux, and consistent with various multi-wavelength diagnostics. Such a high intrinsic to observed flux ratio in addition to an Fe-Kα fluorescence line equivalent width exceeding 2 keV is extreme amongst known bona fide CTK AGN, which we suggest are both due to the high level of obscuration present around IC 3639. Our study demonstrates that broadband spectroscopic modelling with NuSTAR enables large corrections for obscuration to be carried out robustly, and emphasises the need for improved modelling of AGN tori showing intense iron fluorescence.

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BAT AGN spectroscopic survey–II. X-ray emission and high-ionization optical emission lines

Cited by 77 publications

References 56 publications

BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics

BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics

Composite Spectral Energy Distributions and Infrared–Optical Colors of Type 1 and Type 2 Quasars

IC 3639—A NEW BONA FIDE COMPTON-THICK AGN UNVEILED BY NuSTAR

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