The physical scale of the far-infrared emission in the most luminous submillimetre galaxies - II. Evidence for merger-driven star formation

Younger, Joshua D.; Fazio, G. G.; Civano, F.; Gurwell, M. A.; Huang, Jia-Sheng; Iono, Daisuke; Peck, A. B.; Petitpas, G.; Scott, K. S.; Wilner, David J.; Wilson, Grant; Yun, Min S.

doi:10.1111/j.1365-2966.2010.16984.x

Cited by 33 publications

(18 citation statements)

References 170 publications

(337 reference statements)

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“…The horizontal axis shows a deconvolved FWHM of the major axis from two-dimensional Gaussian fitting The results of ADF22 sources are shown. We also show those of previous works (Younger et al 2010;Riechers et al 2014;Ikarashi et al 2015;Simpson et al 2015b). The flux densities at 870 μm (Simpson et al 2015b) and at 890 μm (Younger et al 2010) are scaled to 1.1mm flux density using S 1.1mm /S 870μm = 0.56 and S 1.1mm /S 890μm = 0.58, respectively.…”

Section: Aztecsupporting

confidence: 50%

“…We also show those of previous works (Younger et al 2010;Riechers et al 2014;Ikarashi et al 2015;Simpson et al 2015b). The flux densities at 870 μm (Simpson et al 2015b) and at 890 μm (Younger et al 2010) are scaled to 1.1mm flux density using S 1.1mm /S 870μm = 0.56 and S 1.1mm /S 890μm = 0.58, respectively. We assume a modified black body with typical values for SMGs (spectral index of β = 1.5, dust temperature of 35 K (e.g., Swinbank et al 2014), and z = 2.5).…”

Section: Aztecsupporting

confidence: 50%

“…, significantly lower than the predicted Eddington limit for radiation pressure supported disks (e.g., Elmegreen 1999; Thompson et al 2005;Younger et al 2010;Andrews & Thompson 2011;Riechers et al 2013Riechers et al , 2014. Therefore, starbursts seen in bright SMGs in ADF22 are not Eddington-limited as a whole.…”

Section: Size Measurement and Star Formation Rate Surface Densitymentioning

confidence: 93%

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ALMA Deep Field in SSA22: Source Catalog and Number Counts

Umehata

Tamura

Kohno

et al. 2017

ApJ

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110

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We present results from a deep 2′×3′ (comoving scale of 3.7 Mpc×5.5 Mpc at z = 3) survey at 1.1mm, taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in the SSA22 field. We observe the core region of a z = 3.09 protocluster, achieving a typical rms sensitivity of 60 μJy beam −1 at a spatial resolution of 0 7. We detect 18 robust ALMA sources at a signal-to-noise ratio (S/N)>5. Comparison between the ALMA map and a 1.1mm map, taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE), indicates that three submillimeter sources discovered by the AzTEC/ASTE survey are resolved into eight individual submillimeter galaxies (SMGs) by ALMA. At least 10 of our 18 ALMA SMGs have spectroscopic redshifts of z;3.09, placing them in the protocluster. This shows that a number of dusty starburst galaxies are forming simultaneously in the core of the protocluster. The nine brightest ALMA SMGs with S/N>10 have a median intrinsic angular size of  -+ 0. 32 0.06 0.13 ( -+ 2.4 0.4 1.0 physical kpc at z = 3.09), which is consistent with previous size measurements of SMGs in other fields. As expected, the source counts show a possible excess compared to the counts in the general fields at S 1.1mm 1.0 mJy, due to the protocluster. Our contiguous mm mapping highlights the importance of large-scale structures on the formation of dusty starburst galaxies.

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Section: Aztecsupporting

confidence: 50%

Section: Aztecsupporting

confidence: 50%

Section: Size Measurement and Star Formation Rate Surface Densitymentioning

confidence: 93%

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ALMA Deep Field in SSA22: Source Catalog and Number Counts

Umehata

Tamura

Kohno

et al. 2017

ApJ

Self Cite

110

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“…SMGs contain large amounts of gas, so they should be relatively efficient at converting energy in CR protons into γ -rays and secondary e ± . Furthermore, they are much more extended spatially than the more compact starbursts observed at low redshift (Chapman et al 2004;Tacconi et al 2006;Genzel et al 2008;Law et al 2009;Younger et al 2010). This means that both diffusive and advective escape will be less effective at transporting CR protons out of SMGs, simply because they have to travel farther, further supporting the case for proton calorimetry at multi-TeV energies .…”

Section: Synchrotron the Fir-x-ray Correlation And Submillimeter Gamentioning

confidence: 94%

Diffuse Hard X-Ray Emission in Starburst Galaxies as Synchrotron From Very High Energy Electrons

Lacki

Thompson

2012

ApJ

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The origin of the diffuse hard X-ray (2-10 keV) emission from starburst galaxies is a long-standing problem. We suggest that synchrotron emission of 10-100 TeV electrons and positrons (e ± ) can contribute to this emission, because starbursts have strong magnetic fields. We consider three sources of e ± at these energies: (1) primary electrons directly accelerated by supernova remnants, (2) pionic secondary e ± created by inelastic collisions between cosmic ray (CR) protons and gas nuclei in the dense interstellar medium of starbursts, and (3) pair e ± produced between the interactions between 10 and 100 TeV γ -rays and the intense far-infrared (FIR) radiation fields of starbursts. We create one-zone steady-state models of the CR population in the Galactic center (R 112 pc), NGC 253, M82, and Arp 220's nuclei, assuming a power-law injection spectrum for electrons and protons. We consider different injection spectral slopes, magnetic field strengths, CR acceleration efficiencies, and diffusive escape times, and include advective escape, radiative cooling processes, and secondary and pair e ± . We compare these models to extant radio and GeV and TeV γ -ray data for these starbursts, and calculate the diffuse synchrotron X-ray and inverse Compton (IC) luminosities of these starbursts in the models which satisfy multiwavelength constraints. If the primary electron spectrum extends to ∼PeV energies and has a proton/electron injection ratio similar to the Galactic value, we find that synchrotron emission contributes 2%-20% of their unresolved, diffuse hard X-ray emission. However, there is great uncertainty in this conclusion because of the limited information on the CR electron spectrum at these high energies. IC emission is likewise a minority of the unresolved X-ray emission in these starbursts, from 0.1% in the Galactic center to 10% in Arp 220's nuclei, with the main uncertainty being the starbursts' magnetic field. We also model generic starbursts, including submillimeter galaxies, in the context of the FIR-X-ray relation, finding that anywhere between 0% and 16% of the total hard X-ray emission is synchrotron for different parameters, and up to 2% in the densest starbursts assuming an E −2.2 injection spectrum and a diffusive escape time of 10 Myr (E/3 GeV) −1/2 (h/100 pc). Neutrino observations by IceCube and TeV γ -ray data from HESS, VERITAS, and CTA can further constrain the synchrotron X-ray emission of starbursts. Our models do not constrain the possibility of hard, second components of primary e ± from sources like pulsars in starbursts, which could enhance the synchrotron X-ray emission further.

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“…During such a second, closer interaction, tidal forces can induce shocks covering a large fraction of the galactic disk, which gives the gas a significantly different behavior than that of the stars [169]. Such an inflow fuels the central region of the merger and participates in the nuclear starburst [13,166,210] often observed as an excess of infrared light or a strong nuclear activity [89,136,144,209,248]. [16,103,153,172]).…”

Section: Gas Dynamicsmentioning

confidence: 99%

Tides in Astronomy and Astrophysics

2013

Lecture Notes in Physics

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The physical scale of the far-infrared emission in the most luminous submillimetre galaxies - II. Evidence for merger-driven star formation

Cited by 33 publications

References 170 publications

ALMA Deep Field in SSA22: Source Catalog and Number Counts

ALMA Deep Field in SSA22: Source Catalog and Number Counts

Diffuse Hard X-Ray Emission in Starburst Galaxies as Synchrotron From Very High Energy Electrons

Tides in Astronomy and Astrophysics

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