Quasar host environments: The view from<i>Planck</i>

Verdier, Loïc; Melin, Jean-Baptiste; Bartlett, J. G.; Magneville, C.; Palanque-Delabrouille, N.; Yèche, Ch

doi:10.1051/0004-6361/201527431

Cited by 22 publications

(41 citation statements)

References 78 publications

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“…However, Cen & Safarzadeh (2015) argued that the observed thermal energies can be fully explained via gravitational heating alone, given the large beam sizes of a few arcmin for WMAP and Planck, and the uncertainties in the dust temperature in the calibration of the tSZ maps. More recently, Crichton et al (2016) performed tSZ analyses similar to those by Chatterjee et al and Ruan et al with a smaller-beam experiment (ACT, ∼ 1 arcmin; Swetz et al 2011) and also found a large thermal energy excess, consistent with the results by Dutta Chowdhury & Chatterjee (2017), although the importance of feedback still remains under debate because of the difficulties in analysing and interpreting the tSZ signal in all these analyses (Le Brun et al 2015;Verdier et al 2016;Hill et al 2017, see also the recent findings by Spacek et al 2017a). In detail, extracting conclusive information from the observations of the tSZ effect is difficult because the separation between the actual tSZ signal and that from other contaminants, i.e., thermal radiation from dust, requires a precise (not straightforward) modeling of the emission spectrum at various frequency bands (Cen & Safarzadeh 2015;Greco et al 2015;Ruan et al 2015).…”

Section: Introductionsupporting

confidence: 56%

Revealing the Warm and Hot Halo Baryons via Thomson Scattering of Quasar Light

Mas-Ribas

2018

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The baryonic content and physical properties of the warm and hot (10 5 T 10 7 K) phases of the circumgalactic medium (CGM) are poorly constrained, owing to the lack of observables probing the requisite range of temperature, spatial scale, halo mass, and redshift. The radiation from a luminous quasar produces a spatially extended emission halo resulting from Thomson scattering off of free electrons in the CGM, which can be used to measure the electron density profile, and therefore, the amount of warm and hot baryonic matter present. We predict the resulting surface brightness profiles and show that they are easily detectable in a three hour integration with the James Webb Space Telescope (JWST), out to ∼ 100 physical kpc from the centers of individual hyper-luminous quasars. This electron scattering surface brightness is redshift independent, and the signal-to-noise ratio depends only very weakly on redshift, in principle allowing measurements of the warm and hot CGM into the Epoch of Reionization at z ∼ 6.5. We consider a litany of potential contaminants, and find that for fainter quasars at z 1, extended stellar halos might be of comparable surface brightness. At z > 2, JWST mid-IR observations start to probe rest-frame optical/UV wavelengths implying that scattering by dust grains in the CGM becomes significant, although multi-color observations should be able to distinguish these scenarios given that Thomson scattering is achromatic.

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Section: Introductionsupporting

confidence: 56%

Revealing the Warm and Hot Halo Baryons via Thomson Scattering of Quasar Light

Mas-Ribas

2018

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“…Testing this hypothesis requires observations at submillimetre (submm) wavelengths, as the copious amounts of dust generated from star-formation absorb the rest-frame optical and ultraviolet (UV) light emitted by stars and reradiate it in the far-infrared (IR), observed here on Earth in the submm due to the high redshifts (usually > 2) of these objects. For instance, one can compare the far-IR luminosities of SMGs and QSOs as a proxy of their total dust contents (e.g., Elbaz et al 2010;Hatziminaoglou et al 2010;Dai et al 2012;Leipski et al 2014;Verdier et al 2016). Observations of molecular gas lines (such as CO) in QSOs are also invaluable as they are associated with their host galaxies, allowing one to compare QSOs with their progenitor SMGs (Solomon & Vanden Bout 2005;Carilli et al 2007;Coppin et al 2008;Wang et al 2010;Simpson et al 2012); indeed, it is found that the molecular gas properties of local infrared QSOs, such as the molecular gas mass, star formation efficiency, and molecular linewidths are indistinguishable from those of ultraluminous infrared galaxies (e.g.…”

mentioning

confidence: 99%

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Hill

Chapman

Scott

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A primary goal of the SCUBA-2 Web survey is to perform tomography of the early inter-galactic medium by studying systems containing some of the brightest quasistellar objects (QSOs; 2.5 < z < 3.0) and nearby submillimetre galaxies. As a first step, this paper aims to characterize the galaxies that host the QSOs. To achieve this, a sample of 13 hyper-luminous (L AGN > 10 14 L ) QSOs with previous submillimetre continuum detections were followed up with CO(3-2) observations using the NOEMA interferometer. All but two of the QSOs are detected in CO(3-2); for one non-detection, our observations show a tentative 2σ line at the expected position and redshift, and for the other non-detection we find only continuum flux density an order of magnitude brighter than the other sources. In three of the fields, a companion potentially suitable for tomography is detected in CO line emission within 25 arcsec of the QSO. We derive gas masses, dynamical masses and far-infrared luminosities, and show that the QSOs in our sample have similar properties as compared to less luminous QSOs and SMGs in the literature, despite the fact that their black-hole masses (which are proportional to L AGN ) are 1-2 orders of magnitude larger. We discuss two interpretations of these observations: this is due to selection effects, such as preferential face-on viewing angles and picking out objects in the tail ends of the scatter in host-galaxy mass and blackhole mass relationships; or the black hole masses have been overestimated because the accretion rates are super-Eddington.

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“…However, there is no general consensus as the inferred thermal energies differ substantially among the various studies. One of the main obstacle in this analysis is represented by the strong dust signal which dominates the SED at ν 100 GHz (Crichton et al 2016;Verdier et al 2016;Soergel et al 2017) and creates a degeneracy with the tSZ signal. An additional complication involves distinguishing between the AGN-induced signal and that of the virialized gas in the host dark matter halo, see e.g.…”

Section: Future Outlookmentioning

confidence: 99%

Broadband Spectral Energy Distributions of SDSS-selected Quasars and of Their Host Galaxies: Intense Activity at the Onset of AGN Feedback

Bianchini

Fabbian

Lapi

et al. 2019

ApJ

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We present the mean spectral energy distribution (SED) of a sample of optically selected quasars (QSOs) at redshifts of 1 ≤ z ≤ 5. To derive it, we exploit photometric information from SDSS, UKIDSS, and WISE surveys in combination with a stacking analysis of Herschel, AKARI, and Planck maps at the location of the QSOs. The near-UV and optical parts of the reconstructed mean rest-frame SED are similar to those found in other studies. However, the SED shows an excess at 1-2 µm (when compared to the aforementioned SEDs normalized in the near-UV) and a prominent bump around 4-6 µm, followed by a decrease out to ∼ 20 µm and a subsequent far-IR bump. From the fitted SEDs we estimate the average active galactic nuclei (AGN) luminosity L AGN and star formation rate (SFR) as function of cosmic time, finding typical L AGN ∼ 10 46 − 10 47 erg/s and SFR ∼ 50 − 1000 M /yr. We develop mid-IR based criteria to split the QSO sample, finding that these allow us to move along the average relationship in the SFR vs. L AGN diagram toward increasing AGN luminosities. When interpreted in the context of the in-situ coevolution scenario presented by Lapi et al. (2014), our results suggest that the detection in the far-IR band is an effective criterion to select objects where the star formation is on the verge of being affected by energy/momentum feedback from the central AGN.

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Quasar host environments: The view fromPlanck

Cited by 22 publications

References 78 publications

Revealing the Warm and Hot Halo Baryons via Thomson Scattering of Quasar Light

Revealing the Warm and Hot Halo Baryons via Thomson Scattering of Quasar Light

The SCUBA-2 web survey: I. Observations of CO(3–2) in hyper-luminous QSO fields

Broadband Spectral Energy Distributions of SDSS-selected Quasars and of Their Host Galaxies: Intense Activity at the Onset of AGN Feedback

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