Feedback‐driven Evolution of the Far‐Infrared Spectral Energy Distributions of Luminous and Ultraluminous Infrared Galaxies

Chakrabarti, Sukanya; Cox, Thomas J.; Hernquist, Lars; Hopkins, Philip F.; Robertson, Brant; Matteo, Tiziana Di

doi:10.1086/510113

Cited by 38 publications

(54 citation statements)

References 101 publications

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“…QSOs are thus expected to be the end-product of the rapid growth of SMBHs seen soon after a phase of high star formation, as seen in SMGs (Sanders et al 1988;Granato et al 2001). Although these models claim to be successful in reproducing and Article published by EDP Sciences explaining several observations (Hopkins et al 2005b(Hopkins et al , 2006Li et al 2007;Chakrabarti et al 2007), more observations are necessary to test their predictions, constrain their parameters, and provide a physical base to some of their assumptions (see e.g. Marulli et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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Aims. Short phases of coeval powerful starburst and AGN activity during the lifetimes of the most massive galaxies are predicted by various models of galaxy formation and evolution. In spite of their recurrence and high luminosity, such events are rarely observed. Finding such systems, understanding their nature, and constraining their number density can provide key constraints to galaxy evolutionary models and insights into the interplay between starburst and AGN activities. Methods. We report the discovery of two sources at z = 3.867 and z = 3.427 that exhibit both powerful starburst and AGN activities. They benefit from multi-wavelength data from radio to X rays from the CFHTLS-D1/SWIRE/XMDS surveys. Follow-up optical and near-infrared spectroscopy, and millimeter IRAM/MAMBO observations are also available. We performed a multi-wavelength analysis of their spectral energy distributions with the aim of understanding the origin of their emission and constraining their luminosities. A comparison with other composite systems at similar redshifts from the literature is also presented. Results. The AGN and starburst bolometric luminosities are ∼1013 L . The AGN emission dominates at X ray, optical, mid-infrared wavelengths, and probably also in the radio. The starburst emission dominates in the far-infrared. The estimated star formation rates range from 500 to 3000 M /yr. The AGN near-infrared and X ray emissions are heavily obscured in both sources with an estimated dust extinction A V ≥ 4, and Compton-thick gas column densities. The two sources are the most obscured and most luminous AGNs detected at millimeter wavelengths currently known. Conclusions. The sources presented in this work are heavily obscured QSOs, but their properties are not fully explained by the standard AGN unification model. In one source, the ultraviolet and optical spectra suggest the presence of outflowing gas and shocks, and both sources show emission from hot dust, most likely in the vicinity of the nucleus. Evidence of moderate, AGN-driven radio activity is also found in both sources. Based on the estimated stellar and black hole masses, the two sources lie on the local M BH −M bulge relation. To remain on this relation as they evolve, their star formation rate has to decrease or stop. Our results support evolutionary models that invoke radio feedback such as the star formation quenching mechanism, and suggest that such a mechanism might play a major role also in powerful AGNs.

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Section: Introductionmentioning

confidence: 99%

Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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show abstract

“…We build on these recent developments here by calculating panchromatic SEDs, spanning optical to millimeter wavelengths, of simulations of gas-rich major mergers by using the self-consistent three-dimensional radiative transfer code RADISHE, which treats the scattering, absorption, and reemission of photons from dust grains, with the dust temperature calculated iteratively on the basis of radiative equilibrium (Chakrabarti & Whitney 2008) by using the Lucy temperature algorithm (Lucy 1999). We conduct a multiwavelength analysis of correlations from rest-frame near-infrared to submillimeter bands, as well as infrared X-ray correlations.…”

Section: Introductionmentioning

confidence: 99%

“…We find, therefore, that Li et al (2008) have overemphasized the resolution aspect of their calculation. As discussed in the Appendix and in Chakrabarti & Whitney (2008), the shape of the near-and mid-IR SED is governed in these calculations primarily by the use of the HRH spectrum and our assumptions about the dust-to-gas ratios in the dense and diffuse phases of the ISM. C07 and Chakrabarti & Mckee (2005) explained the shape of the far-IR SED in terms of L/M and AE.…”

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confidence: 99%

An Evolutionary Model for Submillimeter Galaxies

Chakrabarti¹,

Fenner²,

Cox³

et al. 2008

Astrophysical Journal

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We calculate multiwavelength spectral energy distributions (SEDs) from simulations of major galaxy mergers with black hole feedback that produce submillimeter bright galaxies (SMGs), using the self-consistent three-dimensional radiative transfer code RADISHE. These calculations allow us to predict multiwavelength correlations for this important class of galaxies. We review star formation rates, the time evolution of the 850 m fluxes, along with the time evolution of the M BH -M ? relation of the SMGs formed in the mergers. We reproduce correlations for local AGNs observed in Spitzer Space Telescope's IRAC bands, and make definitive predictions for infrared X-ray correlations. Our dynamical approach allows us to directly correlate observed clustering in the data as seen in IRAC color-color plots with the relative amount of time the system spends in a region of color-color space. We also find that this clustering is positively correlated with the stars dominating in their contribution to the total bolometric luminosity. We compare our calculated SEDs to observations of SMGs and find good agreement. We introduce a simple, heuristic classification scheme which we present in terms of the L IR /L X ratios of these galaxies, which may be interpreted as an evolutionary scheme, as these galaxies evolve in L IR /L X while transiting from a X-ray underluminous infrared bright phase (class I, L IR /L X k100), through a quasar phase (class II, L IR /L X $ 25), to a merger remnant (class III, L IR /L X P 10). We find that SMGs are a broader class of systems than starbursts or quasars, traversing the range from class I to class II systems.

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“…We use the self-consistent 3-D Monte Carlo radiative transfer code RADISHE to calculate the emergent SEDs and images through the time outputs of the SPH simulations, as in prior work (Chakrabarti et al 2007;Chakrabarti & Whitney 2009). The radiative transfer methodology is described in Chakrabarti & Whitney (2009;henceforth CW09).…”

Section: Emergent Seds and Imagesmentioning

confidence: 99%

“…For this tracer to be useful, the colors would need to be robust to the choice of star formation (SF) prescription, dust model (or ISM decomposition). This work builds on our earlier work on calculating the emergent SEDs from SPH simulations (Chakrabarti et al 2007;Chakrabarti & Whitney 2009). The choice of ISM decomposition (Jonsson et al 2010;Narayanan et al 2010) will affect the emergent SED, and we are exploring a range of prescriptions to understand the primary dependences.…”

Section: Introductionmentioning

confidence: 98%

Spikes in the SED and ripples in the outskirts of galaxies

Chakrabarti

2011

Proc. IAU

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Abstract. We describe a new method that allows us to quantitatively characterize galactic satellites from analysis of disturbances in outer gas disks, without requiring knowledge of their optical light. We have demonstrated the validity of this method, which we call Tidal Analysis, by applying it to local spirals with known optical companions, including M51 and NGC 1512. These galaxies span the range from having a low mass companion (∼ one-hundredth the mass of the primary galaxy) to a fairly massive companion (∼ one-third the mass of the primary galaxy). This approach has broad implications for many areas of astrophysics -for the indirect detection of dark matter (or dark matter-dominated dwarf galaxies), and for galaxy evolution in its use as a decipher of the dynamical impact of satellites on galactic disks. Here, we present some preliminary results on the emergent SEDs and images, calculated along the time sequence of these dynamical simulations using the 3-D self-consistent Monte Carlo radiative transfer code RADISHE. We explore star formation prescriptions and how they affect the emergent SEDs and images. Our goal is to identify SED colors that are primarily affected by the galaxy's interaction history, and are not significantly affected by the choice of star formation prescription. If successful, we may be able to utilize the emergent UV-IR SED of the primary galaxy to understand its recent interaction history.

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Feedback‐driven Evolution of the Far‐Infrared Spectral Energy Distributions of Luminous and Ultraluminous Infrared Galaxies

Cited by 38 publications

References 101 publications

Obscured and powerful AGN and starburst activities at z ~ 3.5

Obscured and powerful AGN and starburst activities at z ~ 3.5

An Evolutionary Model for Submillimeter Galaxies

Spikes in the SED and ripples in the outskirts of galaxies

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