ERRATUM: “ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6 ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD” (2016, ApJ, 820, 83)

Scoville, N. Z.; Sheth, Kartik; Aussel, H.; Bout, P. A. Vanden; Capak, P.; Bongiorno, A.; Casey, Caitlin M.; Murchikova, Lena; Koda, Jin; Álvarez-Márquez, J.; Lee, N.; Laigle, C.; McCracken, H. J.; Ilbert, O.; Pope, Alexandra; Sanders, D. B.; Chu, J.; Toft, Sune; Ivison, R. J.; Manohar, S.

doi:10.3847/0004-637x/824/1/63

Cited by 225 publications

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“…5.5 to derive the column densities. Then, because of the existing uncertainties in the CO luminosity to gas mass conversion factors, we also calculate the molecular gas masses assuming a Galactic α CO = 6.5 (as in Scoville et al 2016). This means that both the masses and column densities simply increase by a factor of 6.5/0.8 ≈ 8.1, since all the relations are linear.…”

Section: Gas Massmentioning

confidence: 99%

“…We firstly adopt α CO = 0.8 to obtain M H 2 from L 1−0 ; we derive L 1−0 from the detected high-J CO lines using different CO Spectral Line Energy Distribution (SLED). As for the continuum emission, we derive L 850µm (rest-frame luminosity at 850 µm, that is ≈ 353 GHz) from the observed flux density S obs (at λ ≈ 2.1 mm) adopting a MBB model, and then we exploit the empirical L 1−0 ∝ L 850µm relation from Scoville et al (2016) to obtain the CO(1-0) luminosity. We note that this is a pure luminosity relation that does not imply any assumption on the α CO factor.…”

Section: Gas Massmentioning

confidence: 99%

“…However, all these relations show a large scatter (at least ∼1 dex for the FIR luminosity); for simplicity, we then assume the single functional form L 1−0 ∝ L 850µm from Scoville et al (2016), also to compare our results with those of Circosta et al (2019), who have assumed the same relation. Scoville et al (2016) then adopt α CO = 6.5 to calibrate directly the M H 2 ∝ L 850µm relation exploiting both the L 1−0 measurements and L 850µm derived from SPIRE and SCUBA fluxes, finding a ratio α 850µm = L 850µm /M H 2 2 = 6.7×10 19 M −1 erg s −1 Hz −1 . They chose a single value for all galaxies in their samples (i.e., SFGs, local ULIRGs and SMGs) arguing that a lower factor would be inappropriate for a globally distributed molecular gas.…”

Section: Gas Massmentioning

confidence: 99%

“…In particular, measurement of the gas mass, dominated by the molecular component at z 2 (Carilli & Walter 2013), can be achieved with different methods: the most common exploits the low-J transition of CO as a tracer of the total molecular gas mass. An alternative method exploits the monochromatic continuum dust luminosity at 850 µm (L 850µm ): Scoville et al (2016) showed an empirical relation between L 850µm and the CO(1-0) emission line luminosity -valid for local ultraluminous infrared galaxies (ULIRGs, L 8−1000µm 10 12 L ), z∼2 SMGs and local star-forming galaxies -from which they derived a direct relation between L 850µm and the molecular gas mass, assuming a Galactic CO-to-H 2 conversion factor. Once the gas mass and size are measured through high resolution observation, the gas column density can be derived assuming a geometrical configuration.…”

Section: Introductionmentioning

confidence: 99%

“…They performed X-ray spectral fitting to derive the column density responsible for the central obscuration, assuming different spectral models. Then they exploited the available UVto-FIR photometric data to derive the 850 µm flux from spectral energy distribution (SED) fitting, and they converted it into gas mass assuming the L 1−0 ∝ L 850µm Scoville et al (2016) empirical relation and the CO-to-H 2 conversion factor α CO = 0.8 M (K km s −1 pc 2 ) −1 . On the basis of a simple assumption of spherical gas distribution with uniform density, they derived column densities of the host ISM that are comparable with those extracted from the X-ray fitting, and concluded that the ISM likely plays a significant role in the obscuration.…”

Section: Introductionmentioning

confidence: 99%

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Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

D’Amato

Gilli²,

Vignali³

et al. 2020

A&A

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Context. Obscured active galactic nuclei (AGN) represent a significant fraction of the entire AGN population, especially at high redshift (∼70% at z=3-5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at far-IR and submillimeter wavelengths. Studying the physical properties of obscured AGN and their host galaxies is crucial to shedding light on the early stages of a massive system lifetime. Aims. We aim to investigate the contribution of the interstellar medium (ISM) to the obscuration of quasars in a sample of distant highly star forming galaxies and to unveil their morphological and kinematics properties. Methods. We exploit Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 4 observations of the continuum (∼2.1mm) and high-J CO emission of a sample of six X-ray selected, far-IR detected galaxies hosting an obscured AGN at z spec > 2.5 in the 7 Ms Chandra Deep Field-South (CDF-S). We measured the masses and sizes of the dust and molecular gas by fitting the images, visibilities, and spectra, and we derived the gas density and column density on the basis of a uniform sphere geometry. Finally, we compared the measured column densities with those derived from the Chandra X-ray spectra. Results. We detected both the continuum and line emission for three sources for which we measured both the flux density and size. For the undetected sources, we derived an upper limit on the flux density from the root mean square (rms) of the images. We found that the detected galaxies are rich in gas and dust (molecular gas mass in the range <0.5 -2.7 × 10 10 M for α CO = 0.8 and up to ∼ 2 × 10 11 M for α CO = 6.5, and dust mass <0.9 -4.9 × 10 8 M ) and generally compact (gas major axis 2.1-3.0 kpc, dust major axis 1.4-2.7 kpc). The column densities associated with the ISM are on the order of 10 23−24 cm −2 , which is comparable with those derived from the X-ray spectra. For the detected sources we also derived dynamical masses in the range 0.8 -3.7 × 10 10 M . Conclusions. We conclude that the ISM of high redshift galaxies can substantially contribute to nuclear obscuration up to the Compton-thick (> 10 24 cm −2 ) regime. In addition, we found that all the detected sources show a velocity gradient reminding one rotating system, even though two of them show peculiar features in their morphology that can be associated with a chaotic, possibly merging, structure.

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Section: Gas Massmentioning

confidence: 99%

Section: Gas Massmentioning

confidence: 99%

Section: Gas Massmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

D’Amato

Gilli²,

Vignali³

et al. 2020

A&A

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Observational Searches for Star-Forming Galaxies at z > 6

Finkelstein

2016

Publ. Astron. Soc. Aust.

147

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Although the universe at redshifts greater than six represents only the first one billion years (<10%) of cosmic time, the dense nature of the early universe led to vigorous galaxy formation and evolution activity which we are only now starting to piece together. Technological improvements have, over only the past decade, allowed large samples of galaxies at such high redshifts to be collected, providing a glimpse into the epoch of formation of the first stars and galaxies. A wide variety of observational techniques have led to the discovery of thousands of galaxy candidates at z > 6, with spectroscopically confirmed galaxies out to nearly z = 9. Using these large samples, we have begun to gain a physical insight into the processes inherent in galaxy evolution at early times. In this review, I will discuss (i) the selection techniques for finding distant galaxies, including a summary of previous and ongoing ground and space-based searches, and spectroscopic follow-up efforts, (ii) insights into galaxy evolution gleaned from measures such as the rest-frame ultraviolet luminosity function, the stellar mass function, and galaxy star-formation rates, and (iii) the effect of galaxies on their surrounding environment, including the chemical enrichment of the universe, and the reionisation of the intergalactic medium. Finally, I conclude with prospects for future observational study of the distant universe, using a bevy of new state-of-the-art facilities coming online over the next decade and beyond.

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The diagnostic power of radio spectra from star-forming galaxies

Murphy

2019

Proc. IAU

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Radio continuum emission from galaxies is powered by a combination of distinct physical processes, each providing unique diagnostic information. Over frequencies spanning ∼ 1–120 GHz, radio spectra of star-forming galaxies are primarily comprised of: (1) non-thermal synchrotron emission powered by accelerated cosmic-ray electrons/positrons; (2) free-free emission from young massive star-forming (H ii) regions; (3) anomalous microwave emission, which is a dominant, but completely unconstrained, foreground in cosmic microwave background experiments; and (4) cold, thermal dust emission that accounts for most of the dust and total mass content in the interstellar medium in galaxies. In this proceeding, we discuss these key energetic processes that contribute to the radio emission from star-forming galaxies, with an emphasis on frequencies ≳30 GHz, where current investigations of star formation within nearby galaxies show that the free-free emission begins to dominate over non-thermal synchrotron emission. We also discuss how planned radio facilities that will access these frequencies, such as a next-generation Very Large Array (ngVLA), will be transformative to our understanding of the star formation process in galaxies.

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ERRATUM: “ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6 ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD” (2016, ApJ, 820, 83)

Cited by 225 publications

References 0 publications

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

Observational Searches for Star-Forming Galaxies at z > 6

The diagnostic power of radio spectra from star-forming galaxies

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