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G. Wright

Bio: G. Wright is an academic researcher from UK Astronomy Technology Centre. The author has contributed to research in topics: Galaxy & Luminous infrared galaxy. The author has an hindex of 14, co-authored 19 publications receiving 3409 citations.

Papers
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Journal ArticleDOI
Seb Oliver1, James J. Bock2, James J. Bock3, Bruno Altieri4, Alexandre Amblard5, V. Arumugam6, Herve Aussel7, Tom Babbedge8, Alexandre Beelen9, Matthieu Béthermin9, Matthieu Béthermin7, Andrew Blain3, Alessandro Boselli10, C. Bridge3, Drew Brisbin11, V. Buat10, Denis Burgarella10, N. Castro-Rodríguez12, N. Castro-Rodríguez13, Antonio Cava14, P. Chanial7, Michele Cirasuolo15, David L. Clements8, A. Conley16, L. Conversi4, Asantha Cooray3, Asantha Cooray17, C. D. Dowell2, C. D. Dowell3, Elizabeth Dubois1, Eli Dwek18, Simon Dye19, Stephen Anthony Eales20, David Elbaz7, Duncan Farrah1, A. Feltre21, P. Ferrero13, P. Ferrero12, N. Fiolet9, N. Fiolet22, M. Fox8, Alberto Franceschini21, Walter Kieran Gear20, E. Giovannoli10, Jason Glenn16, Yan Gong17, E. A. González Solares23, Matthew Joseph Griffin20, Mark Halpern24, Martin Harwit, Evanthia Hatziminaoglou, Sebastien Heinis10, Peter Hurley1, Ho Seong Hwang7, A. Hyde8, Edo Ibar15, O. Ilbert10, K. G. Isaak25, Rob Ivison6, Rob Ivison15, Guilaine Lagache9, E. Le Floc'h7, L. R. Levenson2, L. R. Levenson3, B. Lo Faro21, Nanyao Y. Lu3, S. C. Madden7, Bruno Maffei26, Georgios E. Magdis7, G. Mainetti21, Lucia Marchetti21, G. Marsden24, J. Marshall3, J. Marshall2, A. M. J. Mortier8, Hien Nguyen2, Hien Nguyen3, B. O'Halloran8, Alain Omont22, Mat Page27, P. Panuzzo7, Andreas Papageorgiou20, H. Patel8, Chris Pearson28, Chris Pearson29, Ismael Perez-Fournon13, Ismael Perez-Fournon12, Michael Pohlen20, Jonathan Rawlings27, Gwenifer Raymond20, Dimitra Rigopoulou29, Dimitra Rigopoulou30, L. Riguccini7, D. Rizzo8, Giulia Rodighiero21, Isaac Roseboom6, Isaac Roseboom1, Michael Rowan-Robinson8, M. Sanchez Portal4, Benjamin L. Schulz3, Douglas Scott24, Nick Seymour27, Nick Seymour31, D. L. Shupe3, A. J. Smith1, Jamie Stevens32, M. Symeonidis27, Markos Trichas33, K. E. Tugwell27, Mattia Vaccari21, Ivan Valtchanov4, Joaquin Vieira3, Marco P. Viero3, L. Vigroux22, Lifan Wang1, Robyn L. Ward1, Julie Wardlow17, G. Wright15, C. K. Xu3, Michael Zemcov2, Michael Zemcov3 
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ∼380deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ∼380 deg^2. Fields range in size from 0.01 to ∼20 deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500 μm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160 μm), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100 000 galaxies at 5σ in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

852 citations

Journal ArticleDOI
Seb Oliver1, James J. Bock2, James J. Bock3, Bruno Altieri4, Alexandre Amblard5, V. Arumugam6, Herve Aussel7, Tom Babbedge8, Alexandre Beelen, Matthieu Béthermin7, Andrew Blain3, Alessandro Boselli9, C. Bridge3, Drew Brisbin10, V. Buat9, Denis Burgarella9, N. Castro-Rodríguez11, N. Castro-Rodríguez12, Antonio Cava13, P. Chanial7, Michele Cirasuolo14, David L. Clements8, A. Conley15, L. Conversi4, Asantha Cooray16, Asantha Cooray3, C. D. Dowell2, C. D. Dowell3, Elizabeth Dubois1, Eli Dwek17, Simon Dye18, Stephen Anthony Eales19, David Elbaz7, Duncan Farrah1, A. Feltre20, P. Ferrero12, P. Ferrero11, N. Fiolet21, M. Fox8, Alberto Franceschini20, Walter Kieran Gear19, E. Giovannoli9, Jason Glenn15, Yan Gong16, E. A. González Solares22, Matthew Joseph Griffin19, Mark Halpern23, Martin Harwit, Evanthia Hatziminaoglou, Sebastien Heinis9, Peter Hurley1, Ho Seong Hwang7, A. Hyde8, Edo Ibar14, O. Ilbert9, K. G. Isaak24, Rob Ivison6, Rob Ivison14, Guilaine Lagache, E. Le Floc'h7, L. R. Levenson3, L. R. Levenson2, B. Lo Faro20, Nanyao Y. Lu3, S. C. Madden7, Bruno Maffei25, Georgios E. Magdis7, G. Mainetti20, Lucia Marchetti20, G. Marsden23, J. Marshall2, J. Marshall3, A. M. J. Mortier8, Hien Nguyen2, Hien Nguyen3, B. O'Halloran8, Alain Omont21, Mat Page26, P. Panuzzo7, Andreas Papageorgiou19, H. Patel8, Chris Pearson27, Chris Pearson28, Ismael Perez-Fournon12, Ismael Perez-Fournon11, Michael Pohlen19, Jonathan Rawlings26, Gwenifer Raymond19, Dimitra Rigopoulou29, Dimitra Rigopoulou28, L. Riguccini7, D. Rizzo8, Giulia Rodighiero20, Isaac Roseboom1, Isaac Roseboom6, Michael Rowan-Robinson8, M. Sanchez Portal4, Benjamin L. Schulz3, Douglas Scott23, Nick Seymour26, Nick Seymour30, D. L. Shupe3, A. J. Smith1, Jamie Stevens31, M. Symeonidis26, Markos Trichas32, K. E. Tugwell26, Mattia Vaccari20, Ivan Valtchanov4, Joaquin Vieira3, Marco P. Viero3, L. Vigroux21, Lifan Wang1, Robyn L. Ward1, Julie Wardlow16, G. Wright14, C. K. Xu3, Michael Zemcov2, Michael Zemcov3 
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ~380 deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey, HerMES, is a legacy program designed to map a set of nested fields totalling ~380 deg^2. Fields range in size from 0.01 to ~20 deg^2, using Herschel-SPIRE (at 250, 350 and 500 \mu m), and Herschel-PACS (at 100 and 160 \mu m), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the re-processed optical and ultra-violet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multi-wavelength understanding of galaxy formation and evolution. The survey will detect of order 100,000 galaxies at 5\sigma in some of the best studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to: facilitate redshift determination; rapidly identify unusual objects; and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include: the total infrared emission of galaxies; the evolution of the luminosity function; the clustering properties of dusty galaxies; and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

707 citations

Journal ArticleDOI
Carlotta Gruppioni1, Francesca Pozzi2, Giulia Rodighiero3, Ivan Delvecchio2, S. Berta4, Lucia Pozzetti1, G. Zamorani1, P. Andreani, Alessandro Cimatti2, O. Ilbert5, E. Le Floc'h, Dieter Lutz4, Benjamin Magnelli4, Lucia Marchetti6, Lucia Marchetti3, Pierluigi Monaco7, Raanan Nordon4, Seb Oliver8, P. Popesso4, L. Riguccini, Isaac Roseboom9, Isaac Roseboom8, David J. Rosario4, Mark Sargent, Mattia Vaccari3, Mattia Vaccari10, Bruno Altieri, H. Aussel, Ángel Bongiovanni11, J. Cepa11, Emanuele Daddi, H. Dominguez-Sanchez11, H. Dominguez-Sanchez1, D. Elbaz, N. M. Foerster Schreiber4, R. Genzel4, Alvaro Iribarrem12, M. Magliocchetti1, Roberto Maiolino13, Albrecht Poglitsch4, A. M. Pérez García, M. Sánchez-Portal, Eckhard Sturm4, Linda J. Tacconi4, Ivan Valtchanov, Alexandre Amblard14, V. Arumugam9, M. Bethermin, James J. Bock15, James J. Bock16, A. Boselli5, V. Buat5, Denis Burgarella5, N. Castro-Rodríguez11, N. Castro-Rodríguez17, Antonio Cava18, P. Chanial, David L. Clements19, A. Conley20, Asantha Cooray21, Asantha Cooray15, C. D. Dowell15, C. D. Dowell16, Eli Dwek22, Stephen Anthony Eales23, Alberto Franceschini3, Jason Glenn20, Matthew Joseph Griffin23, Evanthia Hatziminaoglou, Edo Ibar24, K. G. Isaak25, Rob Ivison24, Rob Ivison9, Guilaine Lagache26, Louis Levenson15, Louis Levenson16, Nanyao Y. Lu15, S. C. Madden, Bruno Maffei27, G. Mainetti3, H. T. Nguyen15, H. T. Nguyen16, B. O'Halloran19, M. J. Page28, P. Panuzzo, Andreas Papageorgiou23, Chris Pearson29, Chris Pearson30, Ismael Perez-Fournon11, Ismael Perez-Fournon17, Michael Pohlen23, Dimitra Rigopoulou30, Dimitra Rigopoulou31, Michael Rowan-Robinson19, Benjamin L. Schulz15, Douglas Scott32, Nick Seymour28, Nick Seymour33, D. L. Shupe15, Anthony J. Smith8, Jamie Stevens34, M. Symeonidis28, Markos Trichas35, K. E. Tugwell28, L. Vigroux36, Lian-Tao Wang8, G. Wright24, C. K. Xu15, Michael Zemcov15, Michael Zemcov16, S. Bardelli1, M. Carollo37, Thierry Contini38, O. Le Fevre5, Simon J. Lilly37, Vincenzo Mainieri, Alvio Renzini1, Marco Scodeggio1, E. Zucca1 
TL;DR: In this article, the authors exploit the deep and extended far-IR data sets (at 70, 100 and 160 μm) of the GPS PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 μm, to derive the evolution of the rest-frame 35-, 60-, 90- and total infrared luminosity functions (LFs) up to z ∼ 4.
Abstract: We exploit the deep and extended far-IR data sets (at 70, 100 and 160 μm) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 μm, to derive the evolution of the rest-frame 35-, 60-, 90- and total infrared (IR) luminosity functions (LFs) up to z ∼ 4. We detect very strong luminosity evolution for the total IR LF (LIR ∝ (1 + z)3.55 ± 0.10 up to z ∼ 2, and ∝ (1 + z)1.62 ± 0.51 at 2 < z ≲ 4) combined with a density evolution (∝(1 + z)−0.57 ± 0.22 up to z ∼ 1 and ∝ (1 + z)−3.92 ± 0.34 at 1 < z ≲ 4). In agreement with previous findings, the IR luminosity density (ρIR) increases steeply to z ∼ 1, then flattens between z ∼ 1 and z ∼ 3 to decrease at z ≳ 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to ρIR. Galaxies occupying the well-established SFR–stellar mass main sequence (MS) are found to dominate both the total IR LF and ρIR at all redshifts, with the contribution from off-MS sources (≥0.6 dex above MS) being nearly constant (∼20 per cent of the total ρIR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 ≤ log(M/M⊙) ≤ 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (≳2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.

461 citations

Journal ArticleDOI
TL;DR: The Herschel Reference Survey (HRS) as discussed by the authors is a key project of the Herschel guaranteed time key project and will be a benchmark study of dust in the nearby universe.
Abstract: The Herschel Reference Survey is a Herschel guaranteed time key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350, and 500 μm. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the center of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass, and environment; (ii) the connection between the dust content and composition and the other phases of the interstellar medium; and (iii) the origin and evolution of dust in galaxies. In this article, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multifrequency data to carry out an analysis of the statistical properties of the sample.

279 citations

Journal ArticleDOI
TL;DR: The Herschel Reference Survey (HRS) as mentioned in this paper is a guaranteed time Herschel key project and will be a benchmark study of dust in the nearby universe and will complement a number of other HRS key projects including large cosmological surveys.
Abstract: The Herschel Reference Survey is a guaranteed time Herschel key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350 and 500 micron. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K-band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the centre of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass and environment, (ii) the connection between the dust content and composition and the other phases of the interstellar medium and (iii) the origin and evolution of dust in galaxies. In this paper, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multi-frequency data to carry out an analysis of the statistical properties of the sample.

276 citations


Cited by
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TL;DR: In this article, the authors review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch.
Abstract: Over the past two decades, an avalanche of data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z~1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ~1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization.

3,104 citations

Journal ArticleDOI
TL;DR: In this article, it was shown that the radiative or quasar mode of feedback can account for the observed proportionality between the central black hole and the host galaxy mass, which can lead to ejection or heating of the gas.
Abstract: Radiation, winds, and jets from the active nucleus of a massive galaxy can interact with its interstellar medium, and this can lead to ejection or heating of the gas. This terminates star formation in the galaxy and stifles accretion onto the black hole. Such active galactic nuclei (AGN) feedback can account for the observed proportionality between the central black hole and the host galaxy mass. Direct observational evidence for the radiative or quasar mode of feedback, which occurs when AGN are very luminous, has been difficult to obtain but is accumulating from a few exceptional objects. Feedback from the kinetic or radio mode, which uses the mechanical energy of radio-emitting jets often seen when AGN are operating at a lower level, is common in massive elliptical galaxies. This mode is well observed directly through X-ray observations of the central galaxies of cool core clusters in the form of bubbles in the hot surrounding medium. The energy flow, which is roughly continuous, heats the hot intraclu...

2,299 citations

Journal ArticleDOI
TL;DR: In this paper, the authors review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch.
Abstract: Over the past two decades, an avalanche of data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z~1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ~1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization.

1,626 citations

Journal ArticleDOI
TL;DR: A review of the outer parts, beyond 1 AU, of protoplanetary disks with a focus on recent IR and (sub)millimeter results can be found in this paper.
Abstract: Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical units are found around almost all low-mass stars shortly after their birth. These disks generally persist for several million years, during which time some material accretes onto the star, some is lost through outflows and photoevaporation, and some condenses into centimeter- and larger-sized bodies or planetesimals. Through observations mainly at IR through millimeter wavelengths, we can determine how common disks are at different ages; measure basic properties including mass, size, structure, and composition; and follow their varied evolutionary pathways. In this way, we see the first steps toward exoplanet formation and learn about the origins of the Solar System. This review addresses observations of the outer parts, beyond 1 AU, of protoplanetary disks with a focus on recent IR and (sub)millimeter results and an eye to the promise of new facilities in the immediate future.

1,366 citations

Journal ArticleDOI
TL;DR: In this paper, the authors examined the infrared (IR) 3-500μm spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data.
Abstract: We present the deepest 100 to 500 μm far-infrared observations obtained with the Herschel Space Observatory as part of the GOODS-Herschel key program, and examine the infrared (IR) 3–500 μm spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data. We determine the projected star formation densities of local galaxies from their radio and mid-IR continuum sizes. We find that the ratio of total IR luminosity to rest-frame 8 μm luminosity, IR8 (≡ L_(IR)^(tot)/L_8), follows a Gaussian distribution centered on IR8 = 4 (σ = 1.6) and defines an IR main sequence for star-forming galaxies independent of redshift and luminosity. Outliers from this main sequence produce a tail skewed toward higher values of IR8. This minority population ( 3 × 10^(10) L_⊙ kpc^(-2)) and a high specific star formation rate (i.e., starbursts). The rest-frame, UV-2700 A size of these distant starbursts is typically half that of main sequence galaxies, supporting the correlation between star formation density and starburst activity that is measured for the local sample. Locally, luminous and ultraluminous IR galaxies, (U)LIRGs (L_(IR)^(tot)≥ 10^(11) L_☉), are systematically in the starburst mode, whereas most distant (U)LIRGs form stars in the “normal” main sequence mode. This confusion between two modes of star formation is the cause of the so-called “mid-IR excess” population of galaxies found at z > 1.5 by previous studies. Main sequence galaxies have strong polycyclic aromatic hydrocarbon (PAH) emission line features, a broad far-IR bump resulting from a combination of dust temperatures (T_(dust) ~ 15–50 K), and an effective T_(dust) ~ 31 K, as derived from the peak wavelength of their infrared SED. Galaxies in the starburst regime instead exhibit weak PAH equivalent widths and a sharper far-IR bump with an effective T_(dust)~ 40 K. Finally, we present evidence that the mid-to-far IR emission of X-ray active galactic nuclei (AGN) is predominantly produced by star formation and that candidate dusty AGNs with a power-law emission in the mid-IR systematically occur in compact, dusty starbursts. After correcting for the effect of starbursts on IR8, we identify new candidates for extremely obscured AGNs.

1,235 citations