Showing papers by "Jason Glenn published in 2011"
University of Colorado Boulder1, McMaster University2, Cardiff University3, European Space Research and Technology Centre4, Ghent University5, University of Manchester6, Centre national de la recherche scientifique7, Imperial College London8, University of California, Irvine9, INAF10, University of Maryland, College Park11
TL;DR: In this paper, the Herschel Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (Herschel SPIRE-FTS) observations of Arp 220, a nearby ultra-luminous infrared galaxy, were presented.
Abstract: We present Herschel Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (Herschel SPIRE-FTS) observations of Arp 220, a nearby ultra-luminous infrared galaxy. The FTS provides continuous spectral coverage from 190 to 670 {mu}m, a wavelength region that is either very difficult to observe or completely inaccessible from the ground. The spectrum provides a good measurement of the continuum and detection of several molecular and atomic species. We detect luminous CO (J = 4-3 to 13-12) and water rotational transitions with comparable total luminosity {approx}2 Multiplication-Sign 10{sup 8} L{sub Sun }; very high-J transitions of HCN (J = 12-11 to 17-16) in absorption; strong absorption features of rare species such as OH{sup +}, H{sub 2}O{sup +}, and HF; and atomic lines of [C I] and [N II]. The modeling of the continuum shows that the dust is warm, with T = 66 K, and has an unusually large optical depth, with {tau}{sub dust} {approx} 5 at 100 {mu}m. The total far-infrared luminosity of Arp 220 is L{sub FIR} {approx} 2 Multiplication-Sign 10{sup 12} L{sub Sun }. Non-LTE modeling of the extinction corrected CO rotational transitions shows that the spectral line energy distribution of CO is fit well by two temperature components:more » cold molecular gas at T {approx} 50 K and warm molecular gas at T {approx} 1350{sup +280}{sub -100} K (the inferred temperatures are much lower if CO line fluxes are not corrected for dust extinction). These two components are not in pressure equilibrium. The mass of the warm gas is 10% of the cold gas, but it dominates the CO luminosity. The ratio of total CO luminosity to the total FIR luminosity is L{sub CO}/L{sub FIR} {approx} 10{sup -4} (the most luminous lines, such as J = 6-5, have L{sub CO,J=6-5}/L{sub FIR} {approx} 10{sup -5}). The temperature of the warm gas is in excellent agreement with the observations of H{sub 2} rotational lines. At 1350 K, H{sub 2} dominates the cooling ({approx}20 L{sub Sun} M{sup -1}{sub Sun }) in the interstellar medium compared to CO ({approx}0.4 L{sub Sun} M{sup -1}{sub Sun }). We have ruled out photodissociation regions, X-ray-dominated regions, and cosmic rays as likely sources of excitation of this warm molecular gas, and found that only a non-ionizing source can heat this gas; the mechanical energy from supernovae and stellar winds is able to satisfy the large energy budget of {approx}20 L{sub Sun} M{sup -1}{sub Sun }. Analysis of the very high-J lines of HCN strongly indicates that they are solely populated by infrared pumping of photons at 14 {mu}m. This mechanism requires an intense radiation field with T > 350 K. We detect a massive molecular outflow in Arp 220 from the analysis of strong P Cygni line profiles observed in OH{sup +}, H{sub 2}O{sup +}, and H{sub 2}O. The outflow has a mass {approx}> 10{sup 7} M{sub Sun} and is bound to the nuclei with velocity {approx}< 250 km s{sup -1}. The large column densities observed for these molecular ions strongly favor the existence of an X-ray luminous AGN (10{sup 44} erg s{sup -1}) in Arp 220.« less
335 citations
TL;DR: The Bolocam Galactic Plane Survey (BGPS) as discussed by the authors is a 1.1 mm continuum survey at 33'' effective resolution of 170 deg2 of the Galactic Plane visible from the northern hemisphere.
Abstract: We present the Bolocam Galactic Plane Survey (BGPS), a 1.1 mm continuum survey at 33'' effective resolution of 170 deg2 of the Galactic Plane visible from the northern hemisphere. The BGPS is one of the first large area, systematic surveys of the Galactic Plane in the millimeter continuum without pre-selected targets. The survey is contiguous over the range –10.5 ≤ l ≤ 90.5, |b| ≤ 0.5. Toward the Cygnus X spiral arm, the coverage was flared to |b| ≤ 1.5 for 75.5 ≤ l ≤ 87.5. In addition, cross-cuts to |b| ≤ 1.5 were made at l= 3, 15, 30, and 31. The total area of this section is 133 deg2. With the exception of the increase in latitude, no pre-selection criteria were applied to the coverage in this region. In addition to the contiguous region, four targeted regions in the outer Galaxy were observed: IC1396 (9 deg2, 97.5 ≤ l ≤ 100.5, 2.25 ≤ b ≤ 5.25), a region toward the Perseus Arm (4 deg2 centered on l = 111, b = 0 near NGC 7538), W3/4/5 (18 deg2, 132.5 ≤ l ≤ 138.5), and Gem OB1 (6 deg2, 187.5 ≤ l ≤ 193.5). The survey has detected approximately 8400 clumps over the entire area to a limiting non-uniform 1σ noise level in the range 11-53 mJy beam–1 in the inner Galaxy. The BGPS source catalog is presented in a previously published companion paper. This paper details the survey observations and data reduction methods for the images. We discuss in detail the determination of astrometric and flux density calibration uncertainties and compare our results to the literature. Data processing algorithms that separate astronomical signals from time-variable atmospheric fluctuations in the data timestream are presented. These algorithms reproduce the structure of the astronomical sky over a limited range of angular scales and produce artifacts in the vicinity of bright sources. Based on simulations, we find that extended emission on scales larger than about 59 is nearly completely attenuated (>90%) and the linear scale at which the attenuation reaches 50% is 38. Comparison with other millimeter-wave data sets implies a possible systematic offset in flux calibration, for which no cause has been discovered. This presentation serves as a companion and guide to the public data release (http://irsa.ipac.caltech.edu/Missions/bolocam.html) through NASA's Infrared Processing and Analysis Center (IPAC) Infrared Science Archive (IRSA). New data releases will be provided through IPAC-IRSA with any future improvements in the reduction. The BGPS provides a complementary long-wavelength spectral band for the ongoing ATLASGAL and Herschel-SPIRE surveys, and an important database and context for imminent observations with SCUBA-2 and ALMA.
326 citations
University of California, Irvine1, California Institute of Technology2, European Space Agency3, University of Edinburgh4, Paris Diderot University5, Jet Propulsion Laboratory6, Aix-Marseille University7, Spanish National Research Council8, University of La Laguna9, Imperial College London10, University of British Columbia11, University of Colorado Boulder12, Goddard Space Flight Center13, Cardiff University14, University of Sussex15, University of Padua16, UK Astronomy Technology Centre17, University of Paris-Sud18, University of Manchester19, Institut d'Astrophysique de Paris20, Rutherford Appleton Laboratory21, University of Lethbridge22, University of Hertfordshire23, University College London24
TL;DR: Excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 μm is reported, and it is found that submillimetre galaxies are located in dark matter haloes with a minimum mass, Mmin, which corresponds to the most efficient mass scale for star formation in the Universe.
Abstract: The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 μm. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, Mmin, such that log10[Mmin/M⊙] = at 350 μm, where M⊙ is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation
139 citations
University of Colorado Boulder1, California Institute of Technology2, University of California, Irvine3, University of Cambridge4, University of Pennsylvania5, Cardiff University6, Rutgers University7, University of Paris-Sud8, Harvard University9, Cornell University10, Aix-Marseille University11, Paris Diderot University12, University of British Columbia13, University of Oxford14, Imperial College London15, University of Sussex16, University of Padua17, Institut d'Astrophysique de Paris18, University of Hertfordshire19, University of Edinburgh20, University of Portsmouth21, University College London22, Rutherford Appleton Laboratory23, University of Lethbridge24, University of La Laguna25, University of California, Davis26
TL;DR: In this article, the authors reported the discovery of a multiply-lensed sub-millimeter galaxy from the HerMES project with an IR luminosity of $1.43 \pm 0.9575.
Abstract: We report the discovery of a bright ($f(250\mum) > 400$ mJy), multiply-lensed submillimeter galaxy \obj\ in {\it Herschel}/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880\mum\ Submillimeter Array observations resolve at least four images with a large separation of $\sim 9\arcsec$. A high-resolution adaptive optics $K_p$ image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of $z=2.9575$, and the lensing model gives a total magnification of $\mu \sim 11 \pm 1$. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, $88 \pm 3$ K. We derive a lensing-corrected total IR luminosity of $(1.43 \pm 0.09) \times 10^{13}\, \mathrm{L}_{\odot}$, implying a star formation rate of $\sim 2500\, \mathrm{M}_{\odot}\, \mathrm{yr}^{-1}$. However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early {\it Herschel} data, and many more are expected as additional data are collected.
120 citations
California Institute of Technology1, University of California, Irvine2, Institut d'Astrophysique de Paris3, University of Maryland, College Park4, Rutgers University5, National Radio Astronomy Observatory6, Cardiff University7, Paris Diderot University8, University of Paris-Sud9, Harvard University10, Jet Propulsion Laboratory11, Cornell University12, Aix-Marseille University13, University of Cambridge14, Imperial College London15, University of Colorado Boulder16, University of Sussex17, University of Padua18, University of Edinburgh19, UK Astronomy Technology Centre20, University College London21, University of Lethbridge22, Rutherford Appleton Laboratory23, Spanish National Research Council24, University of La Laguna25, University of Pennsylvania26
TL;DR: In this article, the authors reported the detection of CO(J = 5 → 4), CO (J = 3 → 2), and CO(j = 1 → 0) emission in the strongly lensed, Herschel/SPIRE-selected submillimeter galaxy (SMG) HERMES J105751.
Abstract: We report the detection of CO(J = 5 → 4), CO(J = 3 → 2), and CO(J = 1 → 0) emission in the strongly lensed, Herschel/SPIRE-selected submillimeter galaxy (SMG) HERMES J105751.1+573027 at z = 2.9574 ± 0.0001, using the Plateau de Bure Interferometer, the Combined Array for Research in Millimeter-wave Astronomy, and the Green Bank Telescope. The observations spatially resolve the molecular gas into four lensed images with a maximum separation of ~9'' and reveal the internal gas dynamics in this system. We derive lensing-corrected CO line luminosities of L'CO(1-0) = (4.17 ± 0.41), L'CO(3-2) = (3.96 ± 0.20), and L'CO(5-4) = (3.45 ± 0.20) × 1010 (μL/10.9)–1 K km s–1 pc2, corresponding to luminosity ratios of r 31 = 0.95 ± 0.10, r 53 = 0.87 ± 0.06, and r 51 = 0.83 ± 0.09. This suggests a total molecular gas mass of M gas = 3.3×1010 (αCO/0.8) (μL/10.9)–1 M ☉. The gas mass, gas mass fraction, gas depletion timescale, star formation efficiency, and specific star formation rate are typical for an SMG. The velocity structure of the gas reservoir suggests that the brightest two lensed images are dynamically resolved projections of the same dust-obscured region in the galaxy that are kinematically offset from the unresolved fainter images. The resolved kinematics appear consistent with the complex velocity structure observed in major, "wet" (i.e., gas-rich) mergers. Major mergers are commonly observed in SMGs and are likely to be responsible for fueling their intense starbursts at high gas consumption rates. This study demonstrates the level of detail to which galaxies in the early universe can be studied by utilizing the increase in effective spatial resolution and sensitivity provided by gravitational lensing.
75 citations
University of Pennsylvania1, Cardiff University2, Paris Diderot University3, Rutgers University4, University of Paris-Sud5, California Institute of Technology6, Jet Propulsion Laboratory7, Cornell University8, Aix-Marseille University9, University of Cambridge10, Imperial College London11, University of Colorado Boulder12, University of California, Irvine13, University of Sussex14, University of Padua15, Institut d'Astrophysique de Paris16, University of Maryland, College Park17, UK Astronomy Technology Centre18, University of Edinburgh19, Japan Aerospace Exploration Agency20, University College London21, University of Lethbridge22, Rutherford Appleton Laboratory23, University of La Laguna24, Spanish National Research Council25, University of British Columbia26
TL;DR: In this article, the authors reported on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES).
Abstract: We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of L FIR = 1.4 × 1013 L , and is lensed by a massive group of galaxies into at least four images with a total magnification of μ = 10.9 ± 0.7. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify a redshift of z = 2.958 ± 0.007 for this source, using the simultaneous detection of four CO emission lines (J = 7 → 6, J = 8 → 7, J = 9 → 8, and J = 10 → 9). Combining the measured line fluxes for these high-J transitions with the J = 1 → 0, J = 3 → 2, and J = 5 → 4 line fluxes measured with the Green Bank Telescope, the Combined Array for Research in Millimeter Astronomy, and the Plateau de Bure Interferometer, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full CO spectral line energy distribution is described well by warm, moderate-density gas with T kin = 86-235 K and cm–3. However, it is possible that the highest-J transitions are tracing a small fraction of very dense gas in molecular cloud cores, and two-component models that include a warm/dense molecular gas phase with T kin ~ 200 K, cm–3 are also consistent with these data. Higher signal-to-noise measurements of the J up ≥ 7 transitions with high spectral resolution, combined with high spatial resolution CO maps, are needed to improve our understanding of the gas excitation, morphology, and dynamics of this interesting high-redshift galaxy.
61 citations
TL;DR: In this paper, a multispecies Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+ was conducted.
Abstract: We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurements with those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct a multi-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T>100 K) gas of H_2 number densities 10^(4.2)-10^(4.9) cm^(–3). Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.
60 citations
Institut d'Astrophysique de Paris1, University of Pennsylvania2, Leiden University3, Max Planck Society4, Open University5, Search for extraterrestrial intelligence6, Paris Diderot University7, Durham University8, University of Oxford9, Rutgers University10, Centre national de la recherche scientifique11, Ghent University12, Imperial College London13, University of California, Irvine14, McGill University15, French Alternative Energies and Atomic Energy Commission16, International School for Advanced Studies17, Cardiff University18, National Radio Astronomy Observatory19, National Institute of Astrophysics, Optics and Electronics20, University of Hertfordshire21, University of Edinburgh22, California Institute of Technology23, Ames Research Center24, INAF25, University of Padua26, Complutense University of Madrid27, University of Nottingham28, Jet Propulsion Laboratory29, University of Colorado Boulder30
TL;DR: Lupu et al. as mentioned in this paper reported observations of the H2O 202 − 111 emission line in SDP17b using the IRAM interferometer equipped with its new 277 −371 GHz receivers.
Abstract: The Herschel survey, H-ATLAS, with its large areal coverage, has recently discovered a number of bright, strongly lensed high-z submillimeter galaxies The strong magnification makes it possible to study molecular species other than CO, which are otherwise difficult to observe in high-z galaxies Among the lensed galaxies already identified by H-ATLAS, the source J0903029-014127B (SDP17b) at z = 2305 is remarkable because of its excitation conditions and a tentative detection of the H2O 202-111 emission line (Lupu et al 2010, ApJ, submitted) We report observations of this line in SDP17b using the IRAM interferometer equipped with its new 277–371 GHz receivers The H2O line is detected at a redshift of z = 23049 ± 00006, with a flux of 78 ± 05 Jy km s-1 and a FWHM of 250 ± 60 km s-1 The new flux is 24 times weaker than the previous tentative detection, although both remain marginally consistent within 16σ The intrinsic line luminosity and ratio of H2O(202 − 111)/CO(8 − 7) are comparable with those of the nearby starburst/enshrouded-AGN Mrk 231, and the ratio I(H2O)/LFIR is even higher, suggesting that SDP17b could also host a luminous AGN The detection of a strong H2O 202 − 111 line in SDP17b implies an efficient excitation mechanism of the water levels that must occur in very dense and warm interstellar gas probably similar to Mrk 231
59 citations
TL;DR: In this paper, the H2O 202-111 emission line was detected at a redshift of z = 2.3049+/-0.0006, with a flux of 7.8+/- 0.5 Jy km s-1 and a FWHM of 250+/-60 km s -1.
Abstract: The Herschel survey, H-ATLAS, with its large areal coverage, has recently discovered a number of bright, strongly lensed high-z submillimeter galaxies. The strong magnification makes it possible to study molecular species other than CO, which are otherwise difficult to observe in high-z galaxies. Among the lensed galaxies already identified by H-ATLAS, the source J090302.9-014127B (SDP.17b) at z = 2.305 is remarkable due to its excitation conditions and a tentative detection of the H2O 202-111 emission line (Lupu et al. 2010). We report observations of this line in SDP.17b using the IRAM interferometer equipped with its new 277- 371GHz receivers. The H2O line is detected at a redshift of z = 2.3049+/-0.0006, with a flux of 7.8+/-0.5 Jy km s-1 and a FWHM of 250+/-60 km s-1. The new flux is 2.4 times weaker than the previous tentative detection, although both remain marginally consistent within 1.6-sigma. The intrinsic line luminosity and ratio of H2O(202-111)/CO8-7 seem comparable with those of the nearby starburst/enshrouded-AGN Mrk 231, suggesting that SDP.17b could also host a luminous AGN. The detection of a strong H2O 202-111 line in SDP.17b implies an efficient excitation mechanism of the water levels that must occur in very dense and warm interstellar gas.
58 citations
University College London1, Cardiff University2, California Institute of Technology3, Jet Propulsion Laboratory4, Cornell University5, Aix-Marseille University6, Paris Diderot University7, Imperial College London8, University of California, Irvine9, University of Sussex10, University of Padua11, University of Colorado Boulder12, UK Astronomy Technology Centre13, University of Edinburgh14, University of Lethbridge15, Rutherford Appleton Laboratory16, Spanish National Research Council17, University of La Laguna18, University of British Columbia19, Institut d'Astrophysique de Paris20
TL;DR: In this paper, the authors investigated the X-ray/IR correlation for star-forming galaxies (SFGs) at z∼ 1, using SPIRE submm data from the recently launched Herschel Space Observatory and deep Xray data from 2-Ms Chandra Deep Field-North survey.
Abstract: For the first time, we investigate the X-ray/infrared (IR) correlation for star-forming galaxies (SFGs) at z∼ 1, using SPIRE submm data from the recently launched Herschel Space Observatory and deep X-ray data from the 2-Ms Chandra Deep Field-North survey. We examine the X-ray/IR correlation in the soft X-ray (SX; 0.5–2 keV) and hard X-ray (HX; 2–10 keV) bands by comparing our z∼ 1 SPIRE-detected SFGs to equivalently IR-luminous (LIR > 1010 L⊙) samples in the local/low-redshift Universe. Our results suggest that the X-ray/IR properties of the SPIRE SFGs are on average similar to those of their local counterparts, as we find no evidence for evolution in the LSX/LIR and LHX/LIR ratios with redshift. We note, however, that at all redshifts, both LSX/LIR and LHX/LIR are strongly dependent on IR luminosity, with luminous and ultraluminous IR galaxies (LIRGs and ULIRGs; LIR > 1011 L⊙) having up to an order of magnitude lower values than normal IR galaxies (LIR < 1011 L⊙). We derive a LSX–LIR relation and confirm the applicability of an existing LHX–LIR relation for both local and distant LIRGs and ULIRGs, consistent with a scenario where X-ray luminosity is correlated with the star formation rate.
54 citations
University of Tokyo1, University of Pennsylvania2, National Institute of Astrophysics, Optics and Electronics3, University of Edinburgh4, University of Colorado Boulder5, California Institute of Technology6, Jet Propulsion Laboratory7, UK Astronomy Technology Centre8, University of Massachusetts Amherst9, Cardiff University10, Illinois Wesleyan University11, Keio University12, Harvard University13
TL;DR: In this paper, an extremely bright (∼37 mJy at 1100 µm and ∼91 µm Jy at 880 µm) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF 1100.001 (hereafter referred to as SXDF1100.001 or Orochi), was detected in the 1100μm observations of the Subaru/XMM-Newton deep field using ASTE.
Abstract: We report on the detection of an extremely bright (∼37 mJy at 1100 μm and ∼91 mJy at 880 μm) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in the 1100 μm observations of the Subaru/XMM–Newton Deep Field using AzTEC on ASTE. Subsequent CARMA 1300-μm and SMA 880-μm observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended [full width at half-maximum (FWHM) of ∼4 arcsec] and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide-band spectrum from 190 to 308 GHz, although no significant emission/absorption lines were found. The derived upper limit to the line-to-continuum flux ratio is 0.1–0.3 (2σ) across the Z-Spec band.
Based on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at z ∼ 3.4 behind a foreground, optically visible (but red) galaxy at z ∼ 1.4. The deduced apparent (i.e., no correction for magnification) infrared luminosity (L_(IR)) and star formation rate (SFR) are 6 × 10^(13) L_⊙ and 11 000 M_⊙ yr^(−1), respectively, assuming that the L_(IR) is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time-scale (3 × 10^7 yr), which is indeed comparable to those in extreme starbursts like the centres of local ultraluminous infrared galaxies (ULIRGs).
TL;DR: In this article, the rest-frame 200-320 μm spectrum of the z = 3.91 quasar APM 08279+5255 was obtained with Z-Spec at the Caltech Submillimeter Observatory.
Abstract: We present the rest-frame 200-320 μm spectrum of the z = 3.91 quasar APM 08279+5255, obtained with Z-Spec at the Caltech Submillimeter Observatory. In addition to the J = 8 → 7 to J = 13 → 12 CO rotational transitions which dominate the CO cooling, we find six transitions of water originating at energy levels ranging up to 643 K. Most are first detections at high redshift, and we have confirmed one transition with CARMA. The CO cooling is well described by our X-ray dominated region (XDR) model, assuming L_(1-100 keV) ~ 1 × 10^(46) erg s^(–1), and that the gas is distributed over a 550-pc size scale, as per the now-favored μ = 4 lensing model. The total observed cooling in water corresponds to 6.5 × 109 L_☉, comparable to that of CO. We compare the water spectrum with that of Mrk 231, finding that the intensity ratios among the high-lying lines are similar, but with a total luminosity scaled up by a factor of ~50. Using this scaling, we estimate an average water abundance relative to H_2 of 1.4 × 10^(–7), a good match to the prediction of the chemical network in the XDR model. As with Mrk 231, the high-lying water transitions are excited radiatively via absorption in the rest-frame far-infrared, and we show that the powerful dust continuum in APM 08279+5255 is more than sufficient to pump this massive reservoir of warm water vapor.
Institut d'Astrophysique de Paris1, California Institute of Technology2, University of California, Irvine3, University of Colorado Boulder4, University of Pennsylvania5, Ames Research Center6, Cardiff University7, University of Paris-Sud8, Harvard University9, Jet Propulsion Laboratory10, Cornell University11, Aix-Marseille University12, Paris Diderot University13, University of British Columbia14, University of Oxford15, Imperial College London16, University of Sussex17, University of Padua18, University of Cambridge19, UK Astronomy Technology Centre20, University of Edinburgh21, University of Hertfordshire22, Japan Aerospace Exploration Agency23, University College London24, Rutherford Appleton Laboratory25, University of Lethbridge26, Spanish National Research Council27, University of La Laguna28, European Space Agency29, University of California, Davis30
TL;DR: In this article, the authors present the results of a gravitational lensing analysis of the bright z s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the HerMES project.
Abstract: We present the results of a gravitational lensing analysis of the bright z s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be μ = 10.9 ± 0.7. We measure the half-light radius R eff of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R eff, * = [2.0 ± 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R eff, gas = [1.1 ± 0.5] kpc) by mapping back in the source plane the CO (J = 5 → 4) transition line emission. The lens modeling yields a relatively large Einstein radius R Ein = 4farcs10 ± 0farcs02, corresponding to a deflector velocity dispersion of [483 ± 16] km s–1. This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z l ~ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f dm(< R Ein) ~ 80%. This fraction reduces to f dm(< R eff, G1 sime 4.5 kpc) ~ 47% within the effective radius of the main deflecting galaxy of stellar mass M *, G1 = [8.5 ± 1.6] × 1011 M ☉. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ~ 0.2 from the Sloan Lens ACS Survey.
University College London1, Cardiff University2, Jet Propulsion Laboratory3, California Institute of Technology4, Cornell University5, Aix-Marseille University6, Paris Diderot University7, Imperial College London8, University of California, Irvine9, University of Sussex10, University of Padua11, University of Colorado Boulder12, UK Astronomy Technology Centre13, University of Edinburgh14, Rutherford Appleton Laboratory15, University of Lethbridge16, University of La Laguna17, Spanish National Research Council18, University of British Columbia19, Institut d'Astrophysique de Paris20
TL;DR: In this paper, the authors investigated the X-ray/IR correlation for star-forming galaxies at z~1, using SPIRE submm data from the recently-launched Herschel Space Observatory and deep X-rays from the 2Ms Chandra deep field north (CDFN) survey.
Abstract: For the first time, we investigate the X-ray/infrared (IR) correlation for star-forming galaxies at z~1, using SPIRE submm data from the recently-launched Herschel Space Observatory and deep X-ray data from the 2Ms Chandra deep field north (CDFN) survey. We examine the X-ray/IR correlation in the soft X-ray (SX, 0.5-2 keV) and hard X-ray (HX, 2-10 keV) bands by comparing our z~1 SPIRE-detected star-forming galaxies (SFGs) to equivalently IR-luminous (L_IR >10^10 L_sun) samples in the local/low redshift Universe. Our results suggest that the X-ray/IR properties of the SPIRE SFGs are on average similar to those of their local counterparts, as we find no evidence for evolution in the L_SX/L_IR and L_HX/L_IR ratios with redshift. We note however, that at all redshifts, both L_SX/L_IR and L_HX/L_IR are strongly dependent on IR luminosity, with luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs,L_IR >10^11 L_sun) having up to an order of magnitude lower values than normal infrared galaxies (L_IR <10^11 L_sun). We derive a L_SX-L_IR relation and confirm the applicability of an existing L_HX-L_IR relation for both local and distant LIRGs and ULIRGs, consistent with a scenario where X-ray luminosity is correlated with the star-formation rate (SFR).
TL;DR: In this paper, the authors present the results of a gravitational lensing analysis of the bright z s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the HerMES project.
Abstract: We present the results of a gravitational lensing analysis of the bright z s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be μ = 10.9 ± 0.7. We measure the half-light radius R eff of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R eff, * = [2.0 ± 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R eff, gas = [1.1 ± 0.5] kpc) by mapping back in the source plane the CO (J = 5 → 4) transition line emission. The lens modeling yields a relatively large Einstein radius R Ein = 410 ± 002, corresponding to a deflector velocity dispersion of [483 ± 16] km s–1. This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z l ~ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f dm(< R Ein) ~ 80%. This fraction reduces to f dm(< R eff, G1 4.5 kpc) ~ 47% within the effective radius of the main deflecting galaxy of stellar mass M *, G1 = [8.5 ± 1.6] × 1011 M ☉. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ~ 0.2 from the Sloan Lens ACS Survey.
University of Sussex1, University of California, Irvine2, California Institute of Technology3, Cardiff University4, Jet Propulsion Laboratory5, Cornell University6, Aix-Marseille University7, Paris Diderot University8, Imperial College London9, University of Padua10, University of Colorado Boulder11, UK Astronomy Technology Centre12, University of Edinburgh13, University College London14, University of Lethbridge15, Rutherford Appleton Laboratory16, University of La Laguna17, Spanish National Research Council18, University of British Columbia19, Institut d'Astrophysique de Paris20
TL;DR: In this paper, a robust study of the cross-correlation between sub-millimetre (submm) sources and sources at lower redshifts was carried out using ancillary data, using two low-redshift samples from the Herschel Multi-tiered Extra-galactic Survey (HerMES) Lockman-Spitzer Wide Area Infrared Extragalactic (SWIRE) field.
Abstract: Cosmic magnification is due to the weak gravitational lensing of sources in the distant Universe by foreground large-scale structure leading to coherent changes in the observed number density of the background sources. Depending on the slope of the background source number counts, cosmic magnification causes a correlation between the background and foreground galaxies, which is unexpected in the absence of lensing if the two populations are spatially disjoint. Previous attempts using submillimetre (submm) sources have been hampered by small number statistics. The large number of sources detected in the Herschel Multi-tiered Extra-galactic Survey (HerMES) Lockman-Spitzer Wide-area Infrared Extragalactic (SWIRE) field enables us to carry out the first robust study of the cross-correlation between submm sources and sources at lower redshifts. Using ancillary data, we compile two low-redshift samples from Sloan Digital Sky Survey (SDSS) and SWIRE with 〈z〉∼ 0.2 and 0.4, respectively, and cross-correlate with two submm samples based on flux density and colour criteria, selecting galaxies preferentially at z∼ 2. We detect cross-correlation on angular scales between ∼1 and 50 arcmin and find clear evidence that this is primarily due to cosmic magnification. A small, but non-negligible signal from intrinsic clustering is likely to be present due to the tails of the redshift distribution of the submm sources overlapping with those of the foreground samples.
Aix-Marseille University1, Paris Diderot University2, Cardiff University3, University of Edinburgh4, Jet Propulsion Laboratory5, California Institute of Technology6, Cornell University7, Imperial College London8, University of California, Irvine9, University of Padua10, University of Colorado Boulder11, University of Cambridge12, University of Sussex13, University College London14, Rutherford Appleton Laboratory15, University of Lethbridge16, University of La Laguna17, Spanish National Research Council18, University of Oxford19, University of British Columbia20, Institut d'Astrophysique de Paris21, UK Astronomy Technology Centre22
TL;DR: In this paper, the spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code CIGALE to estimate physical parameters of high-mass, luminous infrared galaxies.
Abstract: As part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman break galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect a sub-sample of 12 objects at 0.7 2.5. The UV-to-FIR spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code CIGALE to estimate physical parameters. We find that LBGs detected by SPIRE are high-mass, luminous infrared galaxies. It appears that LBGs are located in a triangle-shaped region in the A FUV versus log L FUV = 0 diagram limited by A FUV = 0 at the bottom and by a diagonal following the temporal evolution of the most massive galaxies from the bottom right to the top left of the diagram. This upper envelop can be used as upper limits for the UV dust attenuation as a function of L FUV. The limits of this region are well explained using a closed-box model, where the chemical evolution of galaxies produces metals, which in turn lead to higher dust attenuation when the galaxies age.
TL;DR: In this paper, a robust study of the cross-correlation between sub-mm sources and sources at lower redshifts was carried out using ancillary data, using two low-redshift samples from SDSS and SWIRE with ~ 0.2 and 0.4, respectively.
Abstract: Cosmic magnification is due to the weak gravitational lensing of sources in the distant Universe by foreground large-scale structure leading to coherent changes in the observed number density of the background sources. Depending on the slope of the background source number counts, cosmic magnification causes a correlation between the background and foreground galaxies, which is unexpected in the absence of lensing if the two populations are spatially disjoint. Previous attempts using submillimetre (sub-mm) sources have been hampered by small number statistics. The large number of sources detected in the {\it Herschel} Multi-tiered Extra-galactic Survey (HerMES) Lockman-SWIRE field enables us to carry out the first robust study of the cross-correlation between sub-mm sources and sources at lower redshifts. Using ancillary data we compile two low-redshift samples from SDSS and SWIRE with ~ 0.2 and 0.4, respectively, and cross-correlate with two sub-mm samples based on flux density and colour criteria, selecting galaxies preferentially at z ~ 2. We detect cross-correlation on angular scales between ~1 and 50 arcmin and find clear evidence that this is primarily due to cosmic magnification. A small, but non-negligible signal from intrinsic clustering is likely to be present due to the tails of the redshift distribution of the sub-mm sources overlapping with those of the foreground samples.
University College London1, University of California, Irvine2, University of Edinburgh3, Paris Diderot University4, California Institute of Technology5, Jet Propulsion Laboratory6, Aix-Marseille University7, Spanish National Research Council8, University of La Laguna9, Imperial College London10, University of Colorado Boulder11, European Space Agency12, Goddard Space Flight Center13, Cardiff University14, University of Padua15, University of Cambridge16, UK Astronomy Technology Centre17, University of Paris-Sud18, University of Manchester19, University of Sussex20, Institut d'Astrophysique de Paris21, University of Lethbridge22, Rutherford Appleton Laboratory23, University of British Columbia24, University of Hertfordshire25, Harvard University26
TL;DR: In this article, the authors examined the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of 25 ≤ log(L1.4/W Hz−1) ≤ 26.5.
Abstract: We examine the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of 25 ≤ log(L1.4/W Hz−1) ≤ 26.5 in the extragalactic Spitzer First Look Survey field. We combine Herschel/SPIRE flux densities with Spitzer/Infrared Array Camera and Multiband Imaging Photometer for Spitzer infrared data to obtain total (m) infrared luminosities for these radio sources. We separate our sources into a moderate, 0.4 < z < 0.9, and a high, 1.2 < z < 3.0, redshift sub-sample and we use Spitzer observations of a z < 0.1 3CRR sample as a local comparison. By comparison to numbers from the Square Kilometre Array (SKA) Simulated Skies, we find that our moderate-redshift sample is complete and our high-redshift sample is 14 per cent complete. We constrain the ranges of mean star formation rates (SFRs) to be 3.4–4.2, 18–41 and 80–581 M⊙ yr−1 for the local, moderate- and high-redshift samples, respectively. Hence, we observe an increase in the mean SFR with increasing redshift which we can parametrize as ∼(1 + z)Q, where Q = 4.2 ± 0.8. However, we observe no trends of mean SFR with radio luminosity within the moderate- or high-redshift bins. We estimate that radio-loud active galactic nuclei (AGN) in the high-redshift sample contribute 0.1–0.5 per cent to the total SFR density at that epoch. Hence, if all luminous starbursts host radio-loud AGN we infer a radio-loud phase duty cycle of 0.001–0.005.
University of Colorado Boulder1, McMaster University2, Cardiff University3, European Space Research and Technology Centre4, Ghent University5, University of Manchester6, Centre national de la recherche scientifique7, Imperial College London8, University of California, Irvine9, INAF10, University of Maryland, College Park11
TL;DR: In this paper, the Herschel SPIRE-FTS observations of Arp~220, a nearby ULIRG, were used to detect luminous CO (J = 4-3 to 13-12) and water ladder with comparable total luminosity; very high-J HCN absorption; OH+, H2O+, and HF in absorption; and CI and NII.
Abstract: We present Herschel SPIRE-FTS observations of Arp~220, a nearby ULIRG. The FTS continuously covers 190 -- 670 microns, providing a good measurement of the continuum and detection of several molecular and atomic species. We detect luminous CO (J = 4-3 to 13-12) and water ladders with comparable total luminosity; very high-J HCN absorption; OH+, H2O+, and HF in absorption; and CI and NII. Modeling of the continuum yields warm dust, with T = 66 K, and an unusually large optical depth of ~5 at 100 microns. Non-LTE modeling of the CO shows two temperature components: cold molecular gas at T ~ 50 K and warm molecular gas at T ~1350 K. The mass of the warm gas is 10% of the cold gas, but dominates the luminosity of the CO ladder. The temperature of the warm gas is in excellent agreement with H2 rotational lines. At 1350 K, H2 dominates the cooling (~20 L_sun/M_sun) in the ISM compared to CO (~0.4 L_sun/M_sun). We found that only a non-ionizing source such as the mechanical energy from supernovae and stellar winds can excite the warm gas and satisfy the energy budget of ~20 L_sun/M_sun. We detect a massive molecular outflow in Arp 220 from the analysis of strong P-Cygni line profiles observed in OH+, H2O+, and H2O. The outflow has a mass > 10^{7} M_sun and is bound to the nuclei with velocity < 250 km/s. The large column densities observed for these molecular ions strongly favor the existence of an X-ray luminous AGN (10^{44} ergs/s) in Arp 220.
University of Sussex1, Cardiff University2, Jet Propulsion Laboratory3, California Institute of Technology4, Cornell University5, Aix-Marseille University6, Paris Diderot University7, University of British Columbia8, Imperial College London9, European Space Agency10, University of California, Irvine11, University of Padua12, University of Colorado Boulder13, University of Edinburgh14, UK Astronomy Technology Centre15, University College London16, University of Lethbridge17, Rutherford Appleton Laboratory18, University of La Laguna19, Spanish National Research Council20, University of Warwick21, Commonwealth Scientific and Industrial Research Organisation22, Institut d'Astrophysique de Paris23
TL;DR: In this article, the authors describe the generation of single-band point source catalogues from submillimetre Herschel-SPIRE observations taken as part of the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey (HerMES).
Abstract: We describe the generation of single-band point source catalogues from submillimetre Herschel-SPIRE observations taken as part of the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey (HerMES). Flux densities are found by means of peak-finding and the fitting of a Gaussian point-response function. With highly-confused images, careful checks must be made on the completeness and flux density accuracy of the detected sources. This is done by injecting artificial sources into the images and analysing the resulting catalogues. Measured flux densities at which 50 per cent of injected sources result in good detections at (250, 350, 500) {\mu}m range from (11.6, 13.2, 13.1) mJy to (25.7, 27.1, 35.8) mJy, depending on the depth of the observation (where a `good' detection is taken to be one with positional offset less than one full-width half-maximum of the point-response function, and with the measured flux density within a factor of 2 of the flux density of the injected source). This paper acts as a reference for the 2010 July HerMES public data release.
University of Sussex1, University of Edinburgh2, UK Astronomy Technology Centre3, University of Copenhagen4, University of California, Irvine5, Cardiff University6, Paris Diderot University7, California Institute of Technology8, Jet Propulsion Laboratory9, Aix-Marseille University10, Cornell University11, Spanish National Research Council12, University of La Laguna13, University of British Columbia14, University of Cambridge15, Imperial College London16, European Space Agency17, Goddard Space Flight Center18, University of Padua19, University of Colorado Boulder20, University of Paris-Sud21, University of Manchester22, University of Hawaii at Manoa23, Institut d'Astrophysique de Paris24, University College London25, Rutherford Appleton Laboratory26, University of Lethbridge27, University of Oxford28, University of Hertfordshire29, Harvard University30
TL;DR: In this paper, the potential of submmmm and submm-mm-radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 µm by the SPIRE instrument on Herschel was investigated.
Abstract: We investigate the potential of submm-mm and submm-mm-radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 {\mu}m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm-sources with reliable radio identifications in the GOODS-N and Lockman Hole North fields 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm-sources are adequately described by a modified blackbody with constant optical depth {\tau} = ({
u}/{
u}0)^{\beta} where {\beta} = +1.8 and {
u}0 = c/100 {\mu}m. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation we derive photometric redshift estimates for the 46 SPIRE detected mm-sources. Testing against the 22 sources with known spectroscopic, or good quality optical/near-IR photometric, redshifts we find submm/mm photometric redshifts offer a redshift accuracy of |z|/(1+z) = 0.16 ( = 0.51). Including constraints from the radio-far IR correlation the accuracy is improved to |z|/(1 + z) = 0.15 ( = 0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to ~ 850 {\mu}m selected samples.
TL;DR: In this paper, a multispecies Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+ was conducted.
Abstract: We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurements with those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct a multi-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T > 100 K) gas of H2 number densities 10^4.2 - 10^4.9 cm^-3. Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.
Aix-Marseille University1, Paris Diderot University2, Cardiff University3, University of Edinburgh4, Jet Propulsion Laboratory5, California Institute of Technology6, Cornell University7, Imperial College London8, University of California, Irvine9, University of Padua10, University of Colorado Boulder11, University of Cambridge12, University of Sussex13, University College London14, University of Lethbridge15, Rutherford Appleton Laboratory16, Spanish National Research Council17, University of La Laguna18, University of Oxford19, University of British Columbia20, Institut d'Astrophysique de Paris21, UK Astronomy Technology Centre22
TL;DR: In this article, the spectral energy distributions of the detected objects detected in the rest-frame FIR were investigated using the code CIGALE to estimate physical parameters of high mass, luminous infrared galaxies.
Abstract: As part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman Break Galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect a sub-sample of 12 objects at 0.7 < z < 1.6 and one object at z ~ 2.0.
The ones detected by Herschel SPIRE have redder observed NUV-U and U-R colors than the others, while the undetected ones have colors consistent with average LBGs at z > 2.5. The UV-to-FIR spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code CIGALE to estimate physical parameters. We find that LBGs detected by SPIRE are high mass, luminous infrared galaxies.
It appears that LBGs are located in a triangle-shaped region in the A_FUV vs. Log L_FUV diagram limited by A_FUV=0 at the bottom and by a diagonal following the temporal evolution of the most massive galaxies from the bottom-right to the top-left of the diagram. This upper envelop can be used as upper limits for the UV dust attenuation as a function of L_FUV}. The limits of this region are well explained using a closed-box model, where the chemical evolution of galaxies produces metals, which in turn lead to higher dust attenuation when the galaxies age.