Herschel Survey of the Palomar-Green QSOs at Low Redshift

We investigate the global cold dust properties of 85 nearby (z < 0.5) QSOs, chosen from the Palomar-Green sample of optically luminous quasars. We determine their infrared spectral energy distributions and estimate their rest-frame luminosities by combining Herschel data from 70 to 500 microns with near-infrared and mid-infrared measurements from the Two Micron All Sky Survey (2MASS) and the Wide-Field Infrared Survey Explorer (WISE). In most sources the far-infrared (FIR) emission can be attributed to thermally heated dust. Single temperature modified black body fits to the FIR photometry give an average dust temperature for the sample of 33~K, with a standard deviation of 8~K, and an average dust mass of 7E6 Solar Masses with a standard deviation of 9E6 Solar Masses. Estimates of star-formation that are based on the FIR continuum emission correlate with those based on the 11.3 microns PAH feature, however, the star-formation rates estimated from the FIR continuum are higher than those estimated from the 11.3 microns PAH emission. We attribute this result to a variety of factors including the possible destruction of the PAHs and that, in some sources, a fraction of the FIR originates from dust heated by the active galactic nucleus and by old stars.Comment: accepted for publication in ApJ

The stellar, molecular gas and dust content of the host galaxies of two z~2.8 dust obscured quasars

We present optical through radio observations of the host galaxies of two dust obscured, luminous quasars selected in the mid-infrared, at z=2.62 and z=2.99, including a search for CO emission. Our limits on the CO luminosities are consistent with these objects having masses of molecular gas <~10^10 solar masses, several times less than those of luminous submillimeter-detected galaxies (SMGs) at comparable redshifts. Their near-infrared spectral energy distributions, however, imply that these galaxies have high stellar masses (~10^11-12 solar masses). The relatively small reservoirs of molecular gas and low dust masses are consistent with them being relatively mature systems at high-z.Comment: AJ, in pres

The Spitzer mid-infrared AGN survey. II-the demographics and cosmic evolution of the AGN population

We present luminosity functions derived from a spectroscopic survey of AGN selected from Spitzer Space Telescope imaging surveys. Selection in the mid-infrared is significantly less affected by dust obscuration. We can thus compare the luminosity functions of the obscured and unobscured AGN in a more reliable fashion than by using optical or X-ray data alone. We find that the AGN luminosity function can be well described by a broken power-law model in which the break luminosity decreases with redshift. At high redshifts ($z>1.6$), we find significantly more AGN at a given bolometric luminosity than found by either optical quasar surveys or hard X-ray surveys. The fraction of obscured AGN decreases rapidly with increasing AGN luminosity, but, at least at high redshifts, appears to remain at $\approx 50$\% even at bolometric luminosities $\sim 10^{14}L_{\odot}$. The data support a picture in which the obscured and unobscured populations evolve differently, with some evidence that high luminosity obscured quasars peak in space density at a higher redshift than their unobscured counterparts. The amount of accretion energy in the Universe estimated from this work suggests that AGN contribute about 12\% to the total radiation intensity of the Universe, and a high radiative accretion efficiency $\approx 0.18^{+0.12}_{-0.07}$ is required to match current estimates of the local mass density in black holes.Comment: 14 pages, accepted by Ap

Sensitive VLBI Observations of the z = 4.7 QSO BRI 1202-0725

We present sensitive phase-referenced VLBI results on the radio continuum emission from the z=4.7 double source BRI 1202-0725. The observations were carried out at 1425 MHz using the Very Long Baseline Array (VLBA), the phased Very Large Array (VLA), and the Green Bank Telescope (GBT). Our sensitive VLBI images of BRI 1202-0725 at 0.25 x 0.14 arcsec resolution show a continuum structure in each of its two components. Fitting Gaussian models to these continuum structures yield total flux densities of 315 +/- 38 and 250 +/- 39 microJy, for the northern and the southern components, respectively. The estimated intrinsic brightness temperatures of these continuum structures are about 2 x 10^4 K. Neither component is detected at the full VLBI resolution (29 mas x 7 mas), with a 4 sigma point source upper limit of 40 microJy/beam, or an upper limit to the intrinsic brightness temperature of 6.7 x 10^5 K. The highest angular resolution with at least a 4sigma detection is about 85 mas. At this resolution, the images reveal a single continuum feature in the northern component of BRI 1202-0725, and two continuum features in the southern component, separated by 320 mas. This is similar to the structures seen in the high resolution images of the CO emission. The extent of the observed continuum sources at 1.4 GHz and the derived brightness temperatures are consistent with nuclear starbursts. Moreover, the absence of any compact high-brightness temperature source suggests that thereis no radio-loud AGN in BRI 1202-0725.Comment: 19 pages, 5 figures. Accepted for publication in A

An X-ray jet discovered by Chandra in the z=4.3 radio-selected quasar GB 1508+5714

We report the Chandra discovery of an X-ray jet associated with the redshift 4.3 radio-loud quasar GB 1508+5714. The jet X-ray emission peaks ~2 arcsec to the South-West of the quasar core. We present archival HST WFPC2 data of the quasar field which shows no optical emission at the location of the X-ray jet. We discuss possible emission mechanisms and give constraints to the magnetic field and energy densities for synchrotron radiation or for Compton scattering of the Cosmic Microwave Background radiation as the jet X-ray emission process.Comment: 5 pages, 4 figures, submitted to ApJ. Letters on Aug.13, accepted for publication in ApJ Letters on Oct.

A close look at the dwarf AGN of NGC 4395 : optical and near-IR integral field spectroscopy

Intermediate-mass black holes (103–105 M⊙) in the centre of dwarf galaxies are believed to be analogous to growing active galactic nuclei (AGNs) in the early Universe. Their characterization can provide insight about the early galaxies. We present optical and near-infrared integral field spectroscopy of the inner ∼50 pc of the dwarf galaxy NGC 4395, known to harbour an AGN. NGC 4395 is an ideal candidate to investigate the nature of dwarf AGN, as it is nearby (d ≈ 4.4 Mpc) enough to allow a close look at its nucleus. The optical data were obtained with the Gemini GMOS-IFU covering the 4500 –7300 Å spectral range at a spatial resolution of 10 pc. The J and K-band spectra were obtained with the Gemini NIFS at spatial resolutions of ∼5 pc. The gas kinematics show a compact, rotation disc component with a projected velocity amplitude of 25 kms−1. We estimate a mass of 7.7 × 105 M⊙ inside a radius of 10 pc. From the Hα broad-line component, we estimate the AGN bolometric luminosity as Lbol=(9.9±1.4)×1040 erg s−1 and a mass MBH=(2.5+1.0−0.8)×105 M⊙ for the central black hole. The mean surface mass densities for the ionized and molecular gas are in the ranges (1–2) M⊙ pc−2 and (1–4) × 10−3 M⊙ pc−2 and the average ratio between ionized and hot molecular gas masses is ∼500. The emission-line flux distributions reveal an elongated structure at 24 pc west of the nucleus, which is blueshifted relative to the systemic velocity of the galaxy by ≈30 kms−1. We speculate that this structure is originated by the accretion of a gas-rich small satellite or by a low-metallicity cosmic clou

The [N II] 205μm Emission in Local Luminous Infrared Galaxies

In this paper, we present the measurements of the [N II] 205 μm line for a flux-limited sample of 122 (ultra-)luminous infrared galaxies [(U)LIRGs] and 20 additional normal galaxies, obtained with the Herschel Space Observatory (Herschel). We explore the far-infrared (FIR) color dependence of the [N II] 205 μm (L_([N II]205μm)) to the total infrared (L_(IR)) luminosity ratio, and find that L_([N II]205μm)/L_(IR) only depends modestly on the 70–160 μm flux density ratio (f_(70)/f_(160)) when f_(70)/f_(160) ≾ 0.6, whereas such dependence becomes much steeper for f_(70/f_(160) > 0.6. We also investigate the relation between L_([N II]205μm) and star formation rate (SFR), and show that L_([N II]205μm) has a nearly linear correlation with SFR, albeit the intercept of such a relation varies somewhat with f_(60)/f_(100), consistent with our previous conclusion that [N II] 205 μm emission can serve as an SFR indicator with an accuracy of ~0.4 dex, or ~0.2 dex if f_(60)/f_(100) is known independently. Furthermore, together with the Infrared Space Observatory measurements of [N II], we use a total of ~200 galaxies to derive the local [N II] 205 μm luminosity function (LF) by tying it to the known IR LF with a bivariate method. As a practical application, we also compute the local SFR volume density (ṗ_(SFR)) using the newly derived SFR calibrator and LF. The resulting log ṗ_(SFR) = -1.96 ± 0.11 M_☉ yr^(−1) Mpc^(−3) agrees well with previous studies. Finally, we determine the electron densities (n_e) of the ionized medium for a subsample of 12 (U)LIRGs with both [N II] 205 μm and [N II] 122 μm data, and find that n_e is in the range of ~1–100 cm^(−3), with a median value of 22 cm^(−3)