' spatial resolution allow us to study the relationships between [CII] line emission, star formation rate (SFR), and far-infrared (FIR) emission on spatial scales of $\\sim2$ kpc. In the central $\\sim$4 kpc of HZ4, the [CII]\u002FFIR ratio is $\\sim3\\times10^{-3}$ on global scales as well as on spatially-resolved scales of $\\sim$2 kpc, comparable to the ratio observed in local moderate starburst galaxies such as M82 or M83. For the first time in an individual normal galaxy at this redshift, we find evidence for outflowing gas from the central star-forming region in the direction of the minor-axis of the galaxy. The projected velocity of the outflow is $\\sim400$ km s$^{-1}$, and the neutral gas mass outflow rate is $\\sim3-6$ times higher than the SFR in the central region. Finally, we detect a diffuse component of [CII] emission, or \"[CII]-halo\", that extends beyond the star-forming disk and has a size of $\\sim12$ kpc in diameter. Most likely the outflow, which has a velocity approximately half the escape velocity of the system, is in part responsible for fueling the [CII] extended emission. Together with the kinematic analysis of HZ4 (presented in a forthcoming paper), the analysis supports that HZ4 is a typical star-forming disk at $z\\sim5$ with interstellar medium (ISM) conditions similar to present-day galaxies forming stars at a similar level, driving a galactic outflow that may already play a role in its evolution. ","authors":[{"id":"53f4789fdabfaee2a1df62e8","name":"R. Herrera-Camus"},{"id":"53f43242dabfaee43ec04080","name":"N. Förster Schreiber"},{"id":"560c59dc45cedb3397523d9e","name":"R. Genzel"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f42e3adabfaedd74d41bb6","name":"A. Bolatto"},{"id":"53f5919edabfaedebef8045b","name":"R. L. Davies"},{"id":"53f36f79dabfae4b349bbf03","name":"D. Fisher"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"5405d41ddabfae450f3d7175","name":"T. Naab"},{"id":"53f47065dabfaee4dc875a62","name":"T. Shimizu"},{"id":"56170fed45cedb3397bb4f1b","name":"K. Tadaki"},{"name":"H. Übler"}],"id":"60015aed91e01163e836a2c2","num_citation":0,"order":7,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F21\u002F2101\u002F2101.05279.pdf","title":"A kiloparsec view of a typical star-forming galaxy when the Universe was ~1 Gyr old. Part I. Outflow, halo, and interstellar medium properties","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2101.05279"],"versions":[{"id":"60015aed91e01163e836a2c2","sid":"2101.05279","src":"arxiv","year":2021}],"year":2021},{"abstract":"We report new detections and limits from a NOEMA and ALMA CO(1-0) search for molecular outflows in 13 local galaxies with high far-infrared surface brightness, and combine these with local universe CO outflow results from the literature. The CO line ratios and spatial outflow structure of our targets provide some constraints on the conversion steps from observables to physical quantities such as molecular mass outflow rates. Where available, ratios between outflow emission in higher J CO transitions and in CO(1-0) are typically consistent with excitation R-i1 less than or similar to 1. However, for IRAS 13120 5453, R-31 = 2.10 +\u002F- 0.29 indicates optically thin CO in the outflow. Like much of the outflow literature, we use ff CO(1 0) = 0.8, and we present arguments for using C = 1 in deriving molecular mass outflow rates. (M)over dot(out) = CM(out)v(out)\u002FR-out. We compare the two main methods for molecular outflow detection: CO millimeter interferometry and Herschel OH-based spectroscopic outflow searches. For 26 sources studied with both methods, we find an 80% agreement in detecting vout & 150 km s 1 outflows, and non-matches can be plausibly ascribed to outflow geometry and signal-to-noise ratio. For a published sample of 12 bright ultraluminous infrared galaxies with detailed OH-based outflow modeling, CO outflows are detected in all but one. Outflow masses, velocities, and sizes for these 11 sources agree well between the two methods, and modest remaining di fferences may relate to the di fferent but overlapping regions sampled by CO emission and OH absorption. Outflow properties correlate better with active galactic nucleus (AGN) luminosity and with bolometric luminosity than with far-infrared surface brightness. The most massive outflows are found for systems with current AGN activity, but significant outflows in nonAGN systems must relate to star formation or to AGN activity in the recent past. We report scaling relations for the increase of outflow mass, rate, momentum rate, and kinetic power with bolometric luminosity. Short flow times of similar to 10(6) yr and some sources with resolved multiple outflow episodes support a role of intermittent driving, likely by AGNs.","authors":[{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f438abdabfaee02acdfd1e","name":"E. Sturm"},{"id":"53f44c06dabfaee0d9bca8d8","name":"A. Janssen"},{"id":"53f39fdadabfae4b34ab3035","name":"S. Veilleux"},{"id":"53f45ec2dabfaedd74e4c37b","name":"S. Aalto"},{"name":"C. Cicone"},{"id":"53f42d59dabfaee2a1c7b94e","name":"A. Contursi"},{"id":"56097c9745cedb3396eed897","name":"R.I. Davies"},{"id":"53f43e9ddabfaeb22f4aab33","name":"C. Feruglio"},{"id":"5405ba4ddabfae450f3cafaf","name":"J. Fischer"},{"name":"A. Fluetsch"},{"id":"548959a2dabfae9b401349b4","name":"S. Garcia-Burillo"},{"id":"5440aa01dabfae7d84b9e0e2","name":"R. Genzel"},{"id":"53f433c4dabfaee4dc768dd3","name":"E. González-Alfonso"},{"id":"53f4511adabfaee02ad44561","name":"J. Graciá-Carpio"},{"id":"53f4789fdabfaee2a1df62e8","name":"R. Herrera-Camus"},{"id":"548719c2dabfae8a11fb3604","name":"R. Maiolino"},{"id":"560cafe545cedb339755f6c0","name":"A. Schruba"},{"id":"53f47065dabfaee4dc875a62","name":"T. Shimizu"}],"doi":"10.1051\u002F0004-6361\u002F201936803","id":"5e09aa34df1a9c0c416b8bc6","num_citation":10,"order":0,"pages":{"end":"","start":""},"title":"Molecular outflows in local galaxies: Method comparison and a role of intermittent AGN driving","venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"633"},"versions":[{"id":"5e09aa34df1a9c0c416b8bc6","sid":"2989744709","src":"mag","vsid":"205231332","year":2020},{"id":"5fc6f6e7d75e2ac63d57b6d5","sid":"WOS:000508595600002","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2020}],"year":2020},{"abstract":" Radial velocity monitoring has revealed the presence of moving broad emission lines in some quasars, potentially indicating the presence of a sub-parsec binary system. Phase-referenced, near-infrared interferometric observations could map out the binary orbit by measuring the photocenter difference between a broad emission line and the hot dust continuum. We show that astrometric data over several years may be able to detect proper motions and accelerations, confirming the presence of a binary and constraining system parameters. The brightness, redshifts, and astrometric sizes of current candidates are well matched to the capabilities of the upgraded VLTI\u002FGRAVITY+ instrument, and we identify a first sample of 10 possible candidates. The astrometric signature depends on the morphology and evolution of hot dust emission in supermassive black hole binary systems. Measurements of the photocenter offset may reveal binary motion whether the hot dust emission region is fixed to the inner edge of the circumbinary disk, or moves in response to the changing irradiation pattern from an accreting secondary black hole. ","authors":[{"id":"53f453b8dabfaee43ecb280b","name":"J. Dexter"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"name":"T. T. Shimizu"},{"id":"561db92d45ce1e596486f368","name":"J. Shangguan"},{"id":"560c59dc45cedb3397523d9b","name":"R. I. Davies"},{"id":"53f42cecdabfaeb2acfe3afe","name":"P. T. de Zeeuw"},{"id":"53f438abdabfaee02acdfd1e","name":"E. Sturm"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"53f43242dabfaee43ec04080","name":"N. M. Förster-Schreiber"},{"id":"560c8d4345cedb339754516f","name":"F. Gao"},{"id":"560c59dc45cedb3397523d9e","name":"R. Genzel"},{"id":"53f6348adabfae43b13fa723","name":"S. Gillessen"},{"id":"53f4364adabfaeecd695eccc","name":"O. Pfuhl"},{"id":"54055447dabfae8faa5c322d","name":"L. J. Tacconi"},{"name":"F. Widmann"}],"doi":"10.3847\u002F1538-4357\u002FABC24F","id":"5f8ffa3291e01125c27dde2d","num_citation":0,"order":1,"pages":{"start":"33"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2010\u002F2010.09735.pdf","title":"Determining sub-parsec supermassive black hole binary orbits with infrared interferometry","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2010.09735","https:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.3847\u002F1538-4357\u002Fabc24f\u002Fpdf"],"venue":{"info":{"name":"The Astrophysical Journal"},"issue":"1","volume":"905"},"versions":[{"id":"5f8ffa3291e01125c27dde2d","sid":"2010.09735","src":"arxiv","year":2020},{"id":"600fe749d4150a363c21f027","sid":"3113329333","src":"mag","vsid":"1980519","year":2020}],"year":2020},{"abstract":"To understand the role that active galactic nuclei (AGN) feedback plays in galaxy evolution, we need in-depth studies of the multi-phase structure and energetics of galaxy-wide outflows. In this work, we present new, deep (similar to 50 h) NOEMA CO(1-0) line observations of the molecular gas in the powerful outflow driven by the AGN in the ultra-luminous infrared galaxy IRAS F08572+3915. We spatially resolve the outflow, finding that its most likely configuration is a wide-angle bicone aligned with the kinematic major axis of the rotation disk. The molecular gas in the wind reaches velocities up to approximately +\u002F- 1200 km s(-1) and transports nearly 20% of the molecular gas mass in the system. We detect a second outflow component located similar to 6 kpc northwest from the galaxy moving away at similar to 900 km s(-1), which could be the result of a previous episode of AGN activity. The total mass and energetics of the outflow, which includes contributions from the ionized, neutral, and warm and cold molecular gas phases, is strongly dominated by the cold molecular gas. In fact, the molecular mass outflow rate is higher than the star formation rate, even if we only consider the gas in the outflow that is fast enough to escape the galaxy, which accounts for similar to 40% of the total mass of the outflow. This results in an outflow depletion time for the molecular gas in the central similar to 1.5 kpc region of only similar to 3 Myr, a factor of similar to 2 shorter than the depletion time by star formation activity.","authors":[{"id":"53f4789fdabfaee2a1df62e8","name":"R. Herrera-Camus"},{"id":"53f44c06dabfaee0d9bca8d8","name":"A. Janssen"},{"id":"53f438abdabfaee02acdfd1e","name":"E. Sturm"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f39fdadabfae4b34ab3035","name":"S. Veilleux"},{"id":"54481d4adabfae87b7dd9c48","name":"R. Davies"},{"id":"53f47065dabfaee4dc875a62","name":"T. Shimizu"},{"id":"53f433c4dabfaee4dc768dd3","name":"E. González-Alfonso"},{"name":"D. Rupke"},{"id":"54055447dabfae8faa5c322d","name":"L. Tacconi"},{"id":"5440aa01dabfae7d84b9e0e2","name":"R. Genzel"},{"name":"C. Cicone"},{"id":"548719c2dabfae8a11fb3604","name":"R. Maiolino"},{"id":"53f42d59dabfaee2a1c7b94e","name":"A. Contursi"},{"id":"53f4511adabfaee02ad44561","name":"J. Graciá-Carpio"}],"doi":"10.1051\u002F0004-6361\u002F201936434","id":"5e09aaffdf1a9c0c416cf8ca","num_citation":2,"order":3,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1911\u002F1911.06326.pdf","title":"AGN feedback in a galaxy merger: Multi-phase, galaxy-scale outflows with a fast molecular gas blob ~6 kpc away from IRAS F08572+3915","venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"635"},"versions":[{"id":"5e09aaffdf1a9c0c416cf8ca","sid":"2990889737","src":"mag","vsid":"205231332","year":2020},{"id":"5dd26bb83a55acce59a0e5f1","sid":"1911.06326","src":"arxiv","year":2019},{"id":"5fc6f67cd75e2ac63d5789e0","sid":"WOS:000519109500001","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2020}],"year":2020},{"abstract":"We analyze the angular momenta of massive star-forming galaxies (SFGs) at the peak of the cosmic star formation epoch (z similar to 0.8-2.6). Our sample of similar to 360 log(M-*\u002FM-circle dot) similar to 9.3-11.8 SFGs is mainly based on the KMOS3D and SINS\u002FzC-SINF surveys of H alpha kinematics, and collectively provides a representative subset of the massive star-forming population. The inferred halo scale angular momentum distribution is broadly consistent with that theoretically predicted for their dark matter halos, in terms of mean spin parameter \u003Clambda \u003E similar to 0.037 and its dispersion (sigma(log lambda) similar to 0.2). Spin parameters correlate with the disk radial scale and with their stellar surface density, but do not depend significantly on halo mass, stellar mass, or redshift. Our data thus support the long-standing assumption that on average, even at high redshifts, the specific angular momentum of disk galaxies reflects that of their dark matter halos (j(d) = j(DM)). The lack of correlation between lambda x (j(d)\u002Fj(DM)) and the nuclear stellar density Sigma(*)(1 kpc) favors a scenario where disk-internal angular momentum redistribution leads to \"compaction\" inside massive high-redshift disks. For our sample, the inferred average stellar to dark matter mass ratio is similar to 2%, consistent with abundance matching results. Including the molecular gas, the total baryonic disk to dark matter mass ratio is similar to 5% for halos near 10(12)M(circle dot), which corresponds to 31% of the cosmologically available baryons, implying that high-redshift disks are strongly baryon dominated.","abstract_zh":"","authors":[{"id":"560c494f45cedb33974fcbfb","name":"andreas burkert"},{"id":"53f43242dabfaee43ec04080","name":"n m forster schreiber"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"53f472a9dabfaeecd6a3bb32","name":"p lang"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"},{"id":"53f434d9dabfaedd74d9286b","name":"emily wisnioski"},{"id":"53f44999dabfaee43ec8a7e8","name":"stijn wuyts"},{"name":"k bandara"},{"id":"5613ed3345cedb3397a0bb99","name":"alessandra beifiori"},{"id":"56255abf45cedb33985af720","name":"ralf bender"},{"id":"53f43100dabfaec09f1423ea","name":"gabriel b brammer"},{"name":"j chan"},{"name":"roger l davies"},{"id":"548779c7dabfae9b401346f7","name":"avishai dekel"},{"id":"53f4620ddabfaeb22f52b12a","name":"maximilian h fabricius"},{"id":"5630f0d445ce1e59687c8339","name":"m fossati"},{"id":"53fa0b49dabfae7f97b024ef","name":"shrinivas r kulkarni"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"name":"j t mendel"},{"id":"53f4cfcedabfaeeee2f81089","name":"ivelina momcheva"}],"doi":"10.3847\u002F0004-637X\u002F826\u002F2\u002F214","id":"56d84bc1dabfae2eeedbb3fa","lang":"en","num_citation":3,"order":17,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1510\u002F1510.03262.pdf","title":"The angular momentum distribution and baryon content of star forming galaxies at z~1-3","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1510.03262","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"826"},"versions":[{"id":"56d84bc1dabfae2eeedbb3fa","sid":"2218717928","src":"mag","year":2015},{"id":"5c61094dda56297340b6eec7","sid":"1510.03262","src":"arxiv","year":2016},{"id":"5fc6f8c7d75e2ac63d58fb19","sid":"WOS:000381977900114","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2016}],"year":2016},{"abstract":"Combining the deepest Herschel extragalactic surveys (PEP, GOODS-H, HerMES), and Monte Carlo mock catalogs, we explore the robustness of dust mass estimates based on modeling of broadband spectral energy distributions (SEDs) with two popular approaches: Draine & Li (2007, ApJ, 657, 810; DL07) and a modified blackbody (MBB). We analyze the cause, drivers, and trends of uncertainties and systematics in thorough detail. As long as the observed SED extends to at least 160-200 mu m in the rest frame, M-dust can be recovered with a \u003E3 sigma significance and without the occurrence of systematics. An average offset of a factor similar to 1.5 exists between DL07- and MBB-based dust masses, based on consistent dust properties. The performance of DL07 modeling turns out to be more robust than that of MBB since relative errors on M-dust are more mildly dependent on the maximum covered rest-frame wavelength and are less scattered. At the depth of the deepest Herschel surveys (in the GOODS-S field), it is possible to retrieve dust masses with a signal-to-noise ratio, S\u002FN \u003E= 3 for galaxies on the main sequence of star formation (MS) down to M* similar to 10(10) [M-circle dot] up to z similar to 1. At higher redshift (z \u003C= 2), the same result is only achieved for objects at the tip of the MS or for those objects lying above the tip owing to sensitivity and wavelength coverage limitations. Molecular gas masses, obtained by converting M-dust through the metallicity-dependent gas-to-dust ratio dGDR, are consistent with those based on the scaling of depletion time, tau(dep), and on CO submm spectroscopy. Focusing on CO-detected galaxies at z \u003E 1, the delta(GDR) dependence on metallicity is consistent with the local relation, provided that a sufficient SED coverage is available. Once we established that Herschel-only and sub-mm-only estimates of dust masses can be affected by large uncertainties and possibly systematics in some cases, we combined far-IR Herschel data and sub-mm ALMA expected fluxes to study the advantages of a full SED coverage. The uncertainty on M-dust reduces to \u003C30% for more than 85% of Herschel galaxies, thus potentially facilitating a fast statistical study of M-dust,M-gas for large samples, at least up to z similar to 2.","abstract_zh":"","authors":[{"id":"53f437a2dabfaee02acd565b","name":"s berta"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"name":"natascha foersterschreiber"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"}],"doi":"10.1051\u002F0004-6361\u002F201527746","id":"56d8cb6fdabfae2eee78a4d2","lang":"en","num_citation":56,"order":1,"pages":{"end":"26","start":"1"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1511\u002F1511.05147.pdf","title":"Measures of galaxy dust and gas mass with Herschel photometry and prospects for ALMA","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1511.05147","https:\u002F\u002Farxiv.org\u002Fpdf\u002F1511.05147","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2016A%26A...587A..73B\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2273309","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2273309","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"587"},"versions":[{"id":"56d8cb6fdabfae2eee78a4d2","sid":"2245387497","src":"mag","year":2015},{"id":"5c610958da56297340b71edb","sid":"1511.05147","src":"arxiv","year":2015},{"id":"5ff68d16d4150a363cd460fd","sid":"3104442113","src":"mag","vsid":"205231332","year":2016},{"id":"5fc6f67dd75e2ac63d578af9","sid":"WOS:000371589800084","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2016}],"year":2016},{"abstract":"We use Herschel 70 to 160 mu m images to study the size of the far-infrared emitting region in about 400 local galaxies and quasar (QSO) hosts. The sample includes normal \"main-sequence\" star-forming galaxies, as well as infrared luminous galaxies and PalomarGreen QSOs, with different levels and structures of star formation. Assuming Gaussian spatial distribution of the far-infrared (FIR) emission, the excellent stability of the Herschel point spread function (PSF) enables us to measure sizes well below the PSF width, by subtracting widths in quadrature. We derive scalings of FIR size and surface brightness of local galaxies with FIR luminosity, with distance from the star-forming main-sequence, and with FIR color. Luminosities L-FIR similar to 1011 L-circle dot can be reached with a variety of structures spanning 2 dex in size. Ultraluminous L-FIR greater than or similar to 1012 L-circle dot galaxies far above the main-sequence inevitably have small R-e;70 similar to 0.5 kpc FIR emitting regions with large surface brightness, and can be close to optically thick in the FIR on average over these regions. Compared to these local relations, first ALMA sizes for the dust emission regions in high redshift galaxies, measured at somewhat longer rest wavelengths, suggest larger sizes at the same IR luminosity. We report a remarkably tight relation with 0.15 dex scatter between FIR surface brightness and the ratio of [CII] 158 mu m emission and FIR emission - the so-called [CII]-deficit is more tightly linked to surface brightness than to FIR luminosity or FIR color. Among 33 z \u003C= 0 : 1 PG QSOs with typical L-FIR\u002FL-Bol,(AGN) approximate to 0.1, 19 have a measured 70 mu m half light radius, with median R-e;70 = 1.1 kpc. This is consistent with the FIR size for galaxies with similar L-FIR but lacking a QSO, in accordance with a scenario where the rest FIR emission of these types of QSOs is, in most cases, due to host star formation.","abstract_zh":"","authors":[{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f437a2dabfaee02acd565b","name":"s berta"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"53f43242dabfaee43ec04080","name":"n m forster schreiber"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"id":"53f4789fdabfaee2a1df62e8","name":"r herreracamus"},{"id":"53f42d85dabfaee43ebc6859","name":"hagai netzer"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"},{"id":"56170fed45cedb3397bb4f1b","name":"k tadaki"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"}],"doi":"10.1051\u002F0004-6361\u002F201527706","id":"56d85368dabfae2eee15a2f9","lang":"en","num_citation":0,"order":0,"pages":{"end":"23","start":"1"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1511\u002F1511.02075.pdf","title":"The far-infrared emitting region in local galaxies and QSOs: Size and scaling relations","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1511.02075","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2016A&A...591A.136L\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2327912","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2327912","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"591"},"versions":[{"id":"56d85368dabfae2eee15a2f9","sid":"2110886017","src":"mag","year":2015},{"id":"5c610955da56297340b711af","sid":"1511.02075","src":"arxiv","year":2016},{"id":"5ff68c77d4150a363cd27c48","sid":"3102440489","src":"mag","vsid":"205231332","year":2016},{"id":"5fc6f648d75e2ac63d576723","sid":"WOS:000379141300145","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2016}],"year":2016},{"abstract":"The optical classification of a Seyfert galaxy and whether it is considered X-ray absorbed are often used interchangeably. There are many borderline cases, however, and also numerous examples where the optical and X-ray classifications appear to be in disagreement. In this article we revisit the relation between optical obscuration and X-ray absorption in active galactic nuclei (AGNs). We make use of our \"dust colour\" method to derive the optical obscuration AV, and consistently estimated X-ray absorbing columns using 0.3-150 keV spectral energy distributions. We also take into account the variable nature of the neutral gas column N-H and derive the Seyfert subclasses of all our objects in a consistent way. We show in a sample of 25 local, hard-X-ray detected Seyfert galaxies (log L-X\u002F(erg\u002Fs) approximate to 41 : 5 43 : 5) that there can actually be a good agreement between optical and X-ray classification. If Seyfert types 1.8 and 1.9 are considered unobscured, the threshold between X-ray unabsorbed and absorbed should be chosen at a column N-H = 10(22.3) cm(-2) to be consistent with the optical classification. We find that N-H is related to A(V) and that the N-H\u002FA(V) ratio is approximately Galactic or higher in all sources, as indicated previously. However, in several objects we also see that deviations from the Galactic ratio are only due to a variable X-ray column, showing that (1) deviations from the Galactic N-H\u002FA(V) can be simply explained by dust-free neutral gas within the broad-line region in some sources; that (2) the dust properties in AGNs can be similar to Galactic dust and that (3) the dust colour method is a robust way to estimate the optical extinction towards the sublimation radius in all but the most obscured AGNs.","abstract_zh":"","authors":[{"id":"53f437f5dabfaec09f18b95f","name":"l burtscher"},{"id":"53f5919edabfaedebef8045b","name":"r davies"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"id":"53f4420fdabfaefedbb0750a","name":"michael koss"},{"name":"m y lin"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"name":"p k nandra"},{"id":"53f42d85dabfaee43ebc6859","name":"hagai netzer"},{"name":"g orban de xivry"},{"id":"5406ede4dabfae450f3f7518","name":"c ricci"},{"id":"53f478d5dabfaefedbbb65b6","name":"d j rosario"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"name":"a schnorrmueller"},{"id":"53f3208edabfae9a84453781","name":"amiel sternberg"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"}],"doi":"10.1051\u002F0004-6361\u002F201527575","id":"56d85f59dabfae2eee6fe2a2","lang":"en","num_citation":27,"order":5,"pages":{"end":"7","start":"1"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1511\u002F1511.05566.pdf","title":"On the relation of optical obscuration and X-ray absorption in Seyfert galaxies","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1511.05566","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2016A&A...586A..28B\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2263778","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2263778","https:\u002F\u002Forbi.uliege.be\u002Fhandle\u002F2268\u002F213734","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"586"},"versions":[{"id":"56d85f59dabfae2eee6fe2a2","sid":"2178566002","src":"mag","year":2015},{"id":"5c610959da56297340b7207e","sid":"1511.05566","src":"arxiv","year":2016},{"id":"5ff68b40d4150a363ccebe77","sid":"3098631854","src":"mag","vsid":"205231332","year":2016},{"id":"5fc6f6aed75e2ac63d579d23","sid":"WOS:000369715900039","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2016}],"year":2016},{"abstract":"We present a complete census of all Herschel-detected sources within the six massive lensing clusters of the HST Frontier Fields (HFF). We provide a robust legacy catalogue of 263 sources with Herschel fluxes, primarily based on imaging from the Herschel Lensing Survey and PEP\u002FHerMES Key Programmes. We optimally combine Herschel, Spitzer and WISE infrared (IR) photometry with data from HST, VLA an...","abstract_zh":"","authors":[{"id":"53f460cfdabfaee02ad7e2ee","name":"t d rawle"},{"id":"53f42ffbdabfaee1c0a54a84","name":"b altieri"},{"id":"54082f80dabfae44f086cb55","name":"e egami"},{"id":"53f5ba3bdabfae5793f8045b","name":"p g perezgonzalez"},{"id":"5432fbd6dabfaeb4c6aa3113","name":"f boone"},{"id":"53f7f09cdabfae92b40f5f7e","name":"b clement"},{"id":"53f456c0dabfaee0d9bf588e","name":"r j ivison"},{"id":"53f42df5dabfaee2a1c83aab","name":"j m richard"},{"id":"53f43453dabfaeee22996f6c","name":"w rujopakarn"},{"id":"53f47316dabfaedd74e9bae5","name":"i valtchanov"},{"id":"53f432e7dabfaedf4355ba89","name":"g l walth"},{"id":"54093f84dabfae8faa679c42","name":"benjamin j weiner"},{"id":"5448a8c9dabfae87b7e5bef5","name":"a w blain"},{"id":"53f454fadabfaee2a1d6e98d","name":"miroslava dessaugeszavadsky"},{"id":"548586dddabfae8a11fb2a98","name":"j p kneib"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"5487af05dabfaed7b5fa31da","name":"g rodighiero"},{"id":"53f43d3bdabfaedd74dd67eb","name":"daniel schaerer"},{"id":"543138c3dabfae8f29139869","name":"ian smail"}],"doi":"10.1093\u002Fmnras\u002Fstw712","id":"56d886f0dabfae2eee9579e3","lang":"en","num_citation":16,"order":15,"pages":{"end":"1645","start":"1626"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1508\u002F1508.00586.pdf","title":"A complete census of Herschel-detected infrared sources within the HST Frontier Fields","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1508.00586","https:\u002F\u002Fieeexplore.ieee.org\u002Fdocument\u002F8156487","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"2","volume":"459"},"versions":[{"id":"56d886f0dabfae2eee9579e3","sid":"1822138409","src":"mag","year":2015},{"id":"5c750966f56def97985eb011","sid":"1822138409","src":"mag","vsid":"195663288","year":2016},{"id":"5c610937da56297340b69826","sid":"1508.00586","src":"arxiv","year":2016},{"id":"5f2d7d5a9fced0a24b20ed66","sid":"8156487","src":"ieee","vsid":"8016813","year":2016},{"id":"5fc9affed83c7e914aa16f0f","sid":"WOS:000377471200038","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2016}],"year":2016},{"abstract":"","abstract_zh":"","authors":[{"name":"e gonzalezalfonso"},{"name":"jacqueline fischer"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"name":"j graciacarpio"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"},{"name":"m melendez"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"name":"a poglitsch"},{"name":"susanne aalto"},{"name":"n falstad"},{"id":"53f47638dabfaedd74ea7db9","name":"h w w spoon"},{"id":"53f4b611dabfaed4b677b3ba","name":"d farrah"},{"name":"a blasco"},{"name":"christian henkel"},{"name":"a contursi"},{"id":"53f466ecdabfaeb22f53f87b","name":"ajay verma"},{"name":"marco spaans"},{"id":"54058d75dabfae92b41e27c8","name":"h a smith"},{"id":"53f42c82dabfaedf43509a39","name":"matthew l n ashby"},{"name":"s haileydunsheath"}],"doi":"","id":"56d8945adabfae2eee021638","lang":"en","num_citation":24,"order":6,"pages":{"end":"","start":""},"title":"High-lying OH Absorption, [C_(II)] Deficits, and Extreme L_(FIR)\u002FM_(H2) Ratios in Galaxies","venue":{"issue":"","volume":""},"versions":[{"id":"56d8945adabfae2eee021638","sid":"172414781","src":"mag","year":2015}],"year":2015},{"abstract":"Herschel\u002FPACS observations of 29 local (ultra) luminous infrared galaxies, including both starburst and active galactic nucleus (AGN) dominated sources as diagnosed in the mid-infrared\u002Foptical, show that the equivalent width of the absorbing OH 65 mu m.3\u002F2 J = 9\u002F2-7\u002F2 line (Weq(OH65)) with lower level energy Elow 300 K, is anticorrelated with the [Cii] 158 mu m line to far-infrared luminosity ratio, and correlated with the far-infrared luminosity per unit gas mass and with the 60-to-100 mu m far-infrared color. While all sources are in the active LIR\u002FMH2 \u003E 50L \u002FM mode as derived from previous CO line studies, the OH65 absorption shows a bimodal distribution with a discontinuity at LFIR\u002FMH2 100L \u002FM . In the most buried sources, OH65 probes material partially responsible for the silicate 9.7 mu m absorption. Combined with observations of the OH 71 mu m.1\u002F2 J = 7\u002F2-5\u002F2 doublet (Elow 415 K), radiative transfer models characterized by the equivalent dust temperature, Tdust, and the continuum optical depth at 100 mu m, t100, indicate that strong [C ii] 158 mu m deficits are associated with far-IR thick (t100 0.7, NH 1024 cm-2), warm (Tdust 60 K) structures where the OH 65 mu m absorption is produced, most likely in circumnuclear disks\u002Ftori\u002Fcocoons. With their high LFIR\u002FMH2 ratios and columns, the presence of these structures is expected to give rise to strong [C ii] deficits. Weq(OH65) probes the fraction of infrared luminosity arising from these compact\u002Fwarm environments, which is 30%-50% in sources with high Weq(OH65). Sources with high Weq(OH65) have surface densities of both LIR and MH2 higher than inferred from the half-light (CO or UV\u002Foptical) radius, tracing coherent structures that represent the most buried\u002Factive stage of (circum) nuclear starburst-AGN co-evolution.","abstract_zh":"","authors":[{"id":"5405ba4ddabfae450f3cafaf","name":"j fischer"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f43940dabfaedce554a28d","name":"a poglitsch"},{"id":"53f45ec2dabfaedd74e4c37b","name":"susanne aalto"},{"name":"n falstad"},{"id":"53f47638dabfaedd74ea7db9","name":"h w w spoon"},{"id":"53f4b611dabfaed4b677b3ba","name":"d farrah"},{"id":"53f4503bdabfaee0d9bdb2a5","name":"a blasco"},{"id":"54105abadabfae92b4277dfc","name":"christian henkel"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"53f466ecdabfaeb22f53f87b","name":"a k verma"},{"id":"5448c467dabfae87b7e7613a","name":"marco spaans"},{"id":"54058d75dabfae92b41e27c8","name":"h a smith"},{"id":"53f42c82dabfaedf43509a39","name":"matthew l n ashby"},{"id":"53f42b99dabfaec22b9fb815","name":"s haileydunsheath"},{"id":"54488805dabfae87b7e3d4d6","name":"p van der werf"},{"id":"53f435f9dabfaeb1a7bf0267","name":"r meijerink"},{"id":"560bfbf645cedb339744a30e","name":"r genzel"}],"doi":"10.1088\u002F0004-637X\u002F800\u002F1\u002F69","id":"56d8378ddabfae2eee4a6d55","lang":"en","num_citation":0,"order":3,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F14\u002F1412\u002F1412.4694.pdf","title":"High-lying OH Absorption, [C II] Deficits, and Extreme L FIR\u002FM H2 Ratios in Galaxies","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F800\u002F1\u002F69","https:\u002F\u002Farxiv.org\u002Fabs\u002F1412.4694","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"800"},"versions":[{"id":"56d8378ddabfae2eee4a6d55","sid":"1999477169","src":"mag","year":2015},{"id":"5c6108edda56297340b57fcc","sid":"1412.4694","src":"arxiv","year":2014},{"id":"5fc6f8f0d75e2ac63d590dbc","sid":"WOS:000349236900069","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2015}],"year":2015},{"abstract":"We combine molecular gas masses inferred from CO emission in 500 star-forming galaxies (SFGs) between z = 0 and 3, from the IRAM-COLDGASS, PHIBSS1\u002F2, and other surveys, with gas masses derived from Herschel far-IR dust measurements in 512 galaxy stacks over the same stellar mass\u002Fredshift range. We constrain the scaling relations of molecular gas depletion timescale (t(depl)) and gas to stellar mass ratio (M-mol (gas)\u002FM*) of SFGs near the star formation \"main-sequence\" with redshift, specific star-formation rate (sSFR), and stellar mass (M*). The CO- and dust-based scaling relations agree remarkably well. This suggests that the CO -\u003E H-2 mass conversion factor varies little within +\u002F- 0.6 dex of the main sequence (sSFR(ms, z, M*)), and less than 0.3 dex throughout this redshift range. This study builds on and strengthens the results of earlier work. We find that t(depl) scales as (1 + z)(-0.3) x (sSFR\u002FsSFR(ms, z, M*))(-0.5), with little dependence on M*. The resulting steep redshift dependence of M-mol (gas)\u002FM-* approximate to (1 + z)(3) mirrors that of the sSFR and probably reflects the gas supply rate. The decreasing gas fractions at high M-* are driven by the flattening of the SFR-M-* relation. Throughout the probed redshift range a combination of an increasing gas fraction and a decreasing depletion timescale causes a larger sSFR at constant M-*. As a result, galaxy integrated samples of the M-mol gas-SFR rate relation exhibit a super-linear slope, which increases with the range of sSFR. With these new relations it is now possible to determine M-mol gas with an accuracy of +\u002F- 0.1 dex in relative terms, and +\u002F- 0.2 dex including systematic uncertainties.","abstract_zh":"","authors":[{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f43687dabfaec09f17e02c","name":"amelie saintonge"},{"name":"s berta"},{"id":"53f43264dabfaeb2ac029e0d","name":"b magnelli"},{"id":"560a73c045cedb33970eb6fd","name":"f combes"},{"id":"548959a2dabfae9b401349b4","name":"s garciaburillo"},{"id":"5408c366dabfae44f088415a","name":"r neri"},{"id":"53f42e3adabfaedd74d41bb6","name":"alberto d bolatto"},{"id":"5405ebb4dabfae450f3e1944","name":"t contini"},{"id":"53f449a1dabfaeecd69b9d16","name":"simon j lilly"},{"name":"jeremie boissier"},{"id":"53f43a7ddabfaefedbaef9a9","name":"f boone"},{"id":"561e7ae645ce1e596492c795","name":"nicolas bouche"},{"id":"53f42f49dabfaee4dc731921","name":"f bournaud"},{"id":"560c494f45cedb33974fcbfb","name":"andreas burkert"},{"id":"53f46f9cdabfaedf43669a8a","name":"marcella carollo"},{"id":"560302d645cedb33960a06e2","name":"luis colina"},{"id":"5484aa1edabfae8a11fb21d3","name":"michael c cooper"}],"doi":"10.1088\u002F0004-637X\u002F800\u002F1\u002F20","id":"56d837aadabfae2eee4b36b8","lang":"en","num_citation":244,"order":2,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F14\u002F1409\u002F1409.1171.pdf","title":"Combined CO and Dust Scaling Relations of Depletion Time and Molecular Gas Fractions with Cosmic Time, Specific Star-formation Rate, and Stellar Mass","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F800\u002F1\u002F20","https:\u002F\u002Farxiv.org\u002Fabs\u002F1409.1171","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"800"},"versions":[{"id":"56d837aadabfae2eee4b36b8","sid":"2093117272","src":"mag","year":2015},{"id":"5c6108cbda56297340b5021b","sid":"1409.1171","src":"arxiv","year":2014},{"id":"5fc6f8f0d75e2ac63d590deb","sid":"WOS:000349236900020","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2015}],"year":2015},{"abstract":"We combine two approaches to isolate the AGN luminosity at near-IR wavelengths and relate the near-IR pure AGN luminosity to other tracers of the AGN. Using integral-field spectroscopic data of an archival sample of 51 local AGNs, we estimate the fraction of non-stellar light by comparing the nuclear equivalent width of the stellar 2.3 mu m CO absorption feature with the intrinsic value for each galaxy. We compare this fraction to that derived from a spectral decomposition of the integrated light in the central arcsecond and find them to be consistent with each other. Using our estimates of the near-IR AGN light, we find a strong correlation with presumably isotropic AGN tracers. We show that a significant off set exists between type 1 and type 2 sources in the sense that type 1 sources are 7 (10) times brighter in the near-IR at log L-AGN(MIR) = 42.5 (log L-AGN(X) = 42.5). These off sets only become clear when treating infrared type 1 sources as type 1 AGNs. All AGNs have very red near-to mid-IR dust colors. This, as well as the range of observed near-IR temperatures, can be explained with a simple model with only two free parameters: the obscuration to the hot dust and the ratio between the warm and hot dust areas. We find obscurations of A(V)(hot) = 5 ... 15 mag for infrared type 1 sources and A(V)(hot) = 15 ... 35 mag for type 2 sources. The ratio of hot dust to warm dust areas of about 1000 is nicely consistent with the ratio of radii of the respective regions as found by infrared interferometry.","abstract_zh":"","authors":[{"id":"53f437f5dabfaec09f18b95f","name":"l burtscher"},{"name":"g orban de xivry"},{"id":"53f5919edabfaedebef8045b","name":"r davies"},{"name":"annemieke janssen"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f478d5dabfaefedbbb65b6","name":"d j rosario"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"name":"m y lin"},{"name":"a schnorrmueller"},{"id":"53f3208edabfae9a84453781","name":"amiel sternberg"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"}],"doi":"10.1051\u002F0004-6361\u002F201525817","id":"56d8aa56dabfae2eeead9ce3","lang":"en","num_citation":0,"order":4,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1504\u002F1504.01104.pdf","title":"Obscuration in AGNs: near-infrared luminosity relations and dust colors","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1051\u002F0004-6361\u002F201525817","https:\u002F\u002Farxiv.org\u002Fabs\u002F1504.01104","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"578"},"versions":[{"id":"56d8aa56dabfae2eeead9ce3","sid":"1793198886","src":"mag","year":2015},{"id":"5c61090fda56297340b603f9","sid":"1504.01104","src":"arxiv","year":2015},{"id":"5fc6f6bdd75e2ac63d57a3ee","sid":"WOS:000357502600059","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2015}],"year":2015},{"abstract":"","abstract_zh":"","authors":[{"name":"kenichi tadaki"},{"id":"53f42d4edabfaeb22f407280","name":"kotaro kohno"},{"id":"53f796b4dabfae9060acfaa9","name":"tadayuki kodama"},{"id":"53f4353cdabfaee1c0a93a6b","name":"s ikarashi"},{"id":"53f432e4dabfaedf4355b809","name":"itziar aretxaga"},{"id":"53f437a2dabfaee02acd565b","name":"s berta"},{"name":"k caputi"},{"id":"5448a308dabfae87b7e55271","name":"j s dunlop"},{"id":"53f47559dabfaeee22a8b4f8","name":"bunyo hatsukade"},{"id":"53f7e943dabfae8faa4c2655","name":"masao hayashi"},{"id":"54301535dabfaeca69bc4dd7","name":"d h hughes"},{"id":"53f456c0dabfaee0d9bf588e","name":"r j ivison"},{"name":"takuma izumi"},{"name":"yusei koyama"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"name":"r makiya"},{"id":"54053643dabfae44f07facb2","name":"yuichi matsuda"},{"id":"53f44cdadabfaee2a1d4e970","name":"kouichiro nakanishi"},{"id":"53f43453dabfaeee22996f6c","name":"w rujopakarn"},{"id":"53f448b9dabfaee02ad225d2","name":"yoichi tamura"}],"doi":"","id":"56d84168dabfae2eee8b4680","lang":"en","num_citation":1,"order":14,"pages":{"end":"","start":""},"title":"SXDF-ALMA 1.5 arcmin^2 deep survey. A compact dusty star-forming galaxy at z=2.5","venue":{"issue":"","volume":""},"versions":[{"id":"56d84168dabfae2eee8b4680","sid":"1837640606","src":"mag","year":2015}],"year":2015},{"abstract":"Emission from high-J CO lines in galaxies has long been proposed as a tracer of X-ray dominated regions (XDRs) produced by active galactic nuclei (AGNs). Of particular interest is the question of whether the obscuring torus, which is required by AGN unification models, can be observed via high-J CO cooling lines. Here we report on the analysis of a deep Herschel\u002FPACS observation of an extremely high-J CO transition (40-39) in the Seyfert 2 galaxy NGC 1068. The line was not detected, with a derived 3 sigma upper limit of 2 x 10(-17) W m(-2). We apply an XDR model in order to investigate whether the upper limit constrains the properties of a molecular torus in NGC 1068. The XDR model predicts the CO spectral line energy distributions for various gas densities and illuminating X-ray fluxes. In our model, the CO(40-39) upper limit is matched by gas with densities of similar to 10(6)-10(7) cm(-3), located at 1.6-5 pc from the AGN, with column densities of at least 1025 cm (2). At such high column densities, however, dust absorbs most of the CO(40-39) line emission at lambda = 65.69 mu m. Therefore, even if NGC 1068 has a molecular torus that radiates in the CO(40-39) line, the dust can attenuate the line emission to below the PACS detection limit. The upper limit is thus consistent with the existence of a molecular torus in NGC 1068. In general, we expect that the CO(40-39) is observable in only a few AGN nuclei (if at all), because of the required high gas column density, and absorption by dust.","abstract_zh":"","authors":[{"name":"annemieke janssen"},{"id":"53f43612dabfaee0d9b62745","name":"s bruderer"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"560c59dc45cedb3397523d9b","name":"r i davies"},{"id":"53f42b99dabfaec22b9fb815","name":"s haileydunsheath"},{"id":"53f43940dabfaedce554a28d","name":"a poglitsch"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"},{"id":"5405ba4fdabfae450f3cb2f6","name":"j fischer"},{"id":"53f433c4dabfaee4dc768dd3","name":"e gonzalezalfonso"},{"id":"53f586dedabfaeb1d1f8045c","name":"a sternberg"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"},{"id":"53f466ecdabfaeb22f53f87b","name":"a k verma"},{"id":"53f437f5dabfaec09f18b95f","name":"l burtscher"}],"doi":"10.1088\u002F0004-637X\u002F811\u002F2\u002F74","id":"56d8377cdabfae2eee49f6e1","lang":"en","num_citation":0,"order":9,"pages":{"end":"","start":"74"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1508\u002F1508.07165.pdf","title":"A deep Herschel\u002FPACS observation of CO(40-39) in NGC 1068: a search for the molecular torus","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F811\u002F2\u002F74","https:\u002F\u002Farxiv.org\u002Fabs\u002F1508.07165","https:\u002F\u002Fwww.nrl.navy.mil\u002Frsd\u002Fsites\u002Fwww.nrl.navy.mil.rsd\u002Ffiles\u002FPDFs\u002FJanssen%2B2015.pdf","https:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.1088\u002F0004-637X\u002F811\u002F2\u002F74\u002Fpdf","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2015ApJ...811...74J\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2237108","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2237108","https:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.1088\u002F0004-637X\u002F811\u002F2\u002F74\u002Fmeta","http:\u002F\u002Fiopscience.iop.org\u002Farticle\u002F10.1088\u002F0004-637X\u002F811\u002F2\u002F74\u002Fmeta","http:\u002F\u002Fauthors.library.caltech.edu\u002F62238\u002F","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"811"},"versions":[{"id":"56d8377cdabfae2eee49f6e1","sid":"1898259197","src":"mag","year":2015},{"id":"5c750a87f56def979862a627","sid":"1898259197","src":"mag","vsid":"1980519","year":2015},{"id":"5c61093eda56297340b6b495","sid":"1508.07165","src":"arxiv","year":2015},{"id":"5ff68b69d4150a363ccf2ca4","sid":"3099084677","src":"mag","vsid":"1980519","year":2015},{"id":"5fc6f85ed75e2ac63d58b335","sid":"WOS:000363513800002","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2015}],"year":2015},{"abstract":"We report the detection of far-infrared (FIR) CO rotational emission from nearby active galactic nuclei (AGNs) and starburst galaxies, as well as several merging systems and Ultra-Luminous Infrared Galaxies (ULIRGs). Using the Herschel Photodetector Array Camera and Spectrometer (PACS), we have detected transitions in the J(upp) = 14-30 range. The PACS CO data obtained here provide the first reference of well-sampled FIR extragalactic CO spectral line energy distributions (SLEDs) for this range. We find a large range in the overall SLED shape, even among galaxies of similar type, demonstrating the uncertainties in relying solely on high-J CO diagnostics to characterize the excitation source of a galaxy. Combining our data with low-J line intensities taken from the literature, we present a CO ratio-ratio diagram and discuss its value in distinguishing excitation sources and physical properties of the molecular gas. The position of a galaxy on such a diagram is less a signature of its excitation mechanism, than an indicator of the presence of warm, dense molecular gas. We then quantitatively analyze the CO emission from a subset of the detected sources with single-component and two-component large velocity gradient (LVG) radiative transfer models to fit the CO SLEDs. From these fits we derive the molecular gas mass and the corresponding CO-to-H-2 conversion factor, alpha(CO), for each respective source. For the ULIRGs we find a values in the canonical range 0.4-5M(circle dot) (K km s(-1) pc(2))(-1), while for the other objects, alpha varies between 0.2 and 14. Finally, we compare our best-fit LVG model results with previous studies of the same galaxies and comment on any differences.","abstract_zh":"","authors":[{"name":"natalie mashian"},{"id":"53f438abdabfaee02acdfd1e","name":"e sturm"},{"id":"53f586dedabfaeb1d1f8045c","name":"a sternberg"},{"name":"a j m janssen"},{"id":"53f42b99dabfaec22b9fb815","name":"s haileydunsheath"},{"id":"5405ba4ddabfae450f3cafaf","name":"j c fischer"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"53f433c4dabfaee4dc768dd3","name":"e gonzalezalfonso"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"id":"53f43940dabfaedce554a28d","name":"a poglitsch"},{"id":"54488f36dabfae87b7e43252","name":"sylvain veilleux"},{"id":"560c59dc45cedb3397523d9b","name":"r i davies"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"54055447dabfae8faa5c322d","name":"l j tacconi"},{"id":"53f466ecdabfaeb22f53f87b","name":"a k verma"},{"name":"a weis"},{"id":"53f43536dabfaec22ba7724a","name":"emil polisensky"},{"id":"53f432b2dabfaee02aca3f5a","name":"tomas nikola"}],"doi":"10.1088\u002F0004-637X\u002F802\u002F2\u002F81","id":"56d83793dabfae2eee4a9cb3","lang":"en","num_citation":3,"order":13,"pages":{"end":"","start":"81"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F14\u002F1410\u002F1410.0006.pdf","title":"High-J CO Sleds in Nearby Infrared Bright Galaxies Observed By Herschel\u002FPACS","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F802\u002F2\u002F81","https:\u002F\u002Farxiv.org\u002Fabs\u002F1410.0006","http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2015ApJ...802...81M\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2157691","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2157691","https:\u002F\u002Fauthors.library.caltech.edu\u002F57571\u002F1\u002F0004-637X_802_2_81.pdf","https:\u002F\u002Fauthors.library.caltech.edu\u002F57571\u002F","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"802"},"versions":[{"id":"56d83793dabfae2eee4a9cb3","sid":"1987046985","src":"mag","year":2015},{"id":"5c6108d4da56297340b522f6","sid":"1410.0006","src":"arxiv","year":2015},{"id":"5ff68c23d4150a363cd17b87","sid":"3101491666","src":"mag","vsid":"1980519","year":2015},{"id":"5fc6f8edd75e2ac63d590c70","sid":"WOS:000353014500009","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2015}],"year":2015},{"abstract":"We study the relationship between the structure and star formation rate (SFR) of X-ray selected low and moderate luminosity active galactic nuclei (AGNs) in the two Chandra Deep Fields, using Hubble Space Telescope imaging from the Cosmic Assembly Near Infrared Extragalactic Legacy Survey (CANDELS) and deep far-infrared maps from the PEP+GOODS-Herschel survey. We derive detailed distributions of structural parameters and FIR luminosities from carefully constructed control samples of galaxies, which we then compare to those of the AGNs. At z similar to 1, AGNs show slightly diskier light profiles than massive inactive (non-AGN) galaxies, as well as modestly higher levels of gross galaxy disturbance (as measured by visual signatures of interactions and clumpy structure). In contrast, at z similar to 2, AGNs show similar levels of galaxy disturbance as inactive galaxies, but display a red central light enhancement, which may arise from a more pronounced bulge in AGN hosts or extinguished nuclear light. We undertake a number of tests of both these alternatives, but our results do not strongly favor one interpretation over the other. The mean SFR and its distribution among AGNs and inactive galaxies are similar at z \u003E 1.5. At z \u003C 1, however, clear and significant enhancements are seen in the SFRs of AGNs with bulge-dominated light profiles. These trends suggest an evolution in the relation between nuclear activity and host properties with redshift, towards a minor role for mergers and interactions at z \u003E 1.5.","abstract_zh":"","authors":[{"id":"53f478d5dabfaefedbbb65b6","name":"d j rosario"},{"id":"54871dbbdabfae9b401341f0","name":"daniel h mcintosh"},{"id":"53f476b7dabfaee43ed36c5a","name":"a van der wel"},{"id":"53f44451dabfaeb22f4b7428","name":"j kartaltepe"},{"id":"53f47596dabfaee4dc88aaad","name":"p lang"},{"id":"53f64375dabfaef15b9bf150","name":"p santini"},{"id":"53f44999dabfaee43ec8a7e8","name":"stijn wuyts"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f42d8edabfaedd74d39106","name":"marc rafelski"},{"id":"53f485c1dabfaec09f2a95d7","name":"c villforth"},{"id":"53f35da5dabfae4b34978902","name":"d m alexander"},{"id":"5408973fdabfae450f42bcf5","name":"f e bauer"},{"id":"53f450d4dabfaee0d9bdda84","name":"eric f bell"},{"id":"53f437a2dabfaee02acd565b","name":"s berta"},{"id":"561e6d0f45ce1e596490ce38","name":"w n brandt"},{"id":"53f7ac4cdabfae92b40d5137","name":"christopher j conselice"},{"id":"548779c7dabfae9b401346f7","name":"avishai dekel"},{"id":"53f43cf8dabfaee1c0ad4023","name":"s m faber"},{"id":"53f43354dabfaee43ec10085","name":"henry c ferguson"},{"id":"560c5c9745cedb339752ad9e","name":"r genzel"}],"doi":"10.1051\u002F0004-6361\u002F201423782","id":"56d91f5edabfae2eee9414b7","lang":"en","num_citation":22,"order":7,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F14\u002F1409\u002F1409.5122.pdf","title":"The Host Galaxies of X-Ray Selected Active Galactic Nuclei to z - 2.5: Structure, Star-Formation and Their Relationships from CANDELS and Herschel\u002FPacs","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F1409.5122","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"573"},"versions":[{"id":"56d91f5edabfae2eee9414b7","sid":"2122327383","src":"mag","year":2014},{"id":"5c6108cfda56297340b5131a","sid":"1409.5122","src":"arxiv","year":2014},{"id":"5fc6f6c3d75e2ac63d57a766","sid":"WOS:000346901300013","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2015}],"year":2015},{"abstract":"We describe a complete volume limited sample of nearby active galaxies selected by their 14-195 keV luminosity, and outline its rationale for studying the mechanisms regulating gas inflow and outflow. We also describe a complementary sample of inactive galaxies, selected to match the host galaxy properties. The active sample appears to have no bias in terms of active galactic nucleus (AGN) type, the only difference being the neutral absorbing column, which is two orders of magnitude greater for the Seyfert 2s. In the luminosity range spanned by the sample, log L14-195 keV [erg s(-1)] = 42.4-43.7, the optically obscured and X-ray absorbed fractions are 50%-65%. The similarity of these fractions to more distant spectroscopic AGN samples, although over a limited luminosity range, suggests that the torus does not strongly evolve with redshift. Our sample confirms that X-ray unabsorbed Seyfert 2s are rare, comprising not more than a few percent of the Seyfert 2 population. At higher luminosities, the optically obscured fraction decreases (as expected for the increasing dust sublimation radius), but the X-ray absorbed fraction changes little. We argue that the cold X-ray absorption in these Seyfert 1s can be accounted for by neutral gas in clouds that also contribute to the broad-line region (BLR) emission, and suggest that a geometrically thick neutral gas torus co-exists with the BLR and bridges the gap to the dusty torus.","abstract_zh":"","authors":[{"id":"560c59dc45cedb3397523d9b","name":"r i davies"},{"id":"53f437f5dabfaec09f18b95f","name":"l burtscher"},{"id":"53f478d5dabfaefedbbb65b6","name":"d rosario"},{"id":"5440a770dabfae7d84b9b641","name":"thaisa storchibergmann"},{"id":"53f42d59dabfaee2a1c7b94e","name":"a contursi"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"53f4511adabfaee02ad44561","name":"j graciacarpio"},{"id":"53f42e27dabfaee1c0a3dad7","name":"e k s hicks"},{"name":"annemieke janssen"},{"id":"53f7cd19dabfae8faa4b6492","name":"michael koss"},{"name":"m y lin"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"},{"id":"53f36b16dabfae4b349ac3bb","name":"witold maciejewski"},{"name":"f mullersanchez"},{"name":"g orban de xivry"},{"id":"5406ede4dabfae450f3f7518","name":"c ricci"},{"id":"53f449c3dabfaeb22f4cdc53","name":"rogemar a riffel"},{"id":"53f467d1dabfaee2a1db4a31","name":"m schartmann"},{"name":"a schnorrmuller"},{"id":"53f586dedabfaeb1d1f8045c","name":"a sternberg"}],"doi":"10.1088\u002F0004-637X\u002F806\u002F1\u002F127","id":"56d837a7dabfae2eee4b1d8e","lang":"en","num_citation":36,"order":11,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1505\u002F1505.00536.pdf","title":"Insights on the Dusty Torus and Neutral Torus from Optical and X-ray Obscuration in a Complete Volume Limited Hard X-ray AGN Sample","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F806\u002F1\u002F127","https:\u002F\u002Farxiv.org\u002Fabs\u002F1505.00536","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"806"},"versions":[{"id":"56d837a7dabfae2eee4b1d8e","sid":"1656044093","src":"mag","year":2015},{"id":"5c610917da56297340b62590","sid":"1505.00536","src":"arxiv","year":2015},{"id":"5fc6f8e9d75e2ac63d590a66","sid":"WOS:000356810300127","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2015}],"year":2015},{"abstract":"","abstract_zh":"","authors":[{"name":"emily wisnioski"},{"id":"53f43242dabfaee43ec04080","name":"n m forster schreiber"},{"id":"53f44999dabfaee43ec8a7e8","name":"stijn wuyts"},{"name":"eva wuyts"},{"name":"k bandara"},{"name":"david j wilman"},{"id":"560c59dc45cedb3397523d9e","name":"r genzel"},{"id":"56255abf45cedb33985af720","name":"ralf bender"},{"id":"53f5919edabfaedebef8045b","name":"r davies"},{"name":"m fossati"},{"name":"p lang"},{"name":"j t mendel"},{"id":"5613ed3345cedb3397a0bb99","name":"alessandra beifiori"},{"id":"53f43100dabfaec09f1423ea","name":"gabriel b brammer"},{"name":"j chan"},{"id":"53f4620ddabfaeb22f52b12a","name":"maximilian h fabricius"},{"id":"53f478fadabfaee1c0ba92e5","name":"y fudamoto"},{"id":"53fa0b49dabfae7f97b024ef","name":"shrinivas r kulkarni"},{"id":"53f42cb7dabfaedce54bb6dd","name":"j kurk"},{"id":"5434ea82dabfaebba587d892","name":"d lutz"}],"doi":"","id":"56d837a2dabfae2eee4b007e","lang":"en","num_citation":32,"order":19,"pages":{"end":"","start":""},"title":"The KMOS3D Survey: Design, First Results, and the Evolution of Galaxy Kinematics from 0.7 ≤ z ≤ 2.7","venue":{"info":{"name":"The Astrophysical Journal"},"issue":"","volume":""},"versions":[{"id":"56d837a2dabfae2eee4b007e","sid":"2167012389","src":"mag","year":2015}],"year":2015}],"profilePubsTotal":395,"profilePatentsPage":1,"profilePatents":[],"profilePatentsTotal":6,"profilePatentsEnd":true,"profileProjectsPage":0,"profileProjects":null,"profileProjectsTotal":null,"newInfo":null,"checkDelPubs":[]}};