The far-infrared-radio relationship at high and low redshift

Vlahakis, C.; Eales, Stephen Anthony; Dunne, L.

doi:10.1111/j.1365-2966.2007.12007.x

Cited by 45 publications

(56 citation statements)

References 47 publications

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“…A possible way to overcome this resolution problem is by taking advantage of the observed correlation between the radio synchrotron and FIR emission in star-forming galaxies (van der Kruit 1971;Condon et al 1982;Helou et al 1985;Garrett 2002;Appleton et al 2004;Beelen et al 2006), which also seems to hold for SMGs out to z ∼ 3 (Kovács et al 2006;Vlahakis et al 2007;Ibar et al 2008;Michałowski et al 2009). Thanks to this FIR-radio correlation, radio interferometric observations can be used as a high-resolution proxy for the rest-frame FIR emission observed in the sub-mm.…”

Section: Fig 1 Summary Of the Results Presented Inmentioning

confidence: 99%

“…Given the low resolution and poor positional accuracy of the sub-mm map, it is very difficult to confirm the connection between SMM J04542-0301 and the optical/NIR lensed images. However, high resolution radio interferometric observations can help to establish this connection thanks to the FIR-radio correlation, which has being found to be valid for SMGs (Kovács et al 2006;Vlahakis et al 2007;Ibar et al 2008;Michałowski et al 2009). …”

Section: Discussionmentioning

confidence: 99%

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Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

Alba

Koopmans²,

Garrett³

et al. 2010

A&A

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Context. SMM J04542-0301 is an extended (∼1 ) submm source located near the core of the cluster MS0451.6-0305. It has been suggested that part of its emission arises from the interaction between a LBG and two EROs at z ∼ 2.9 that are multiply-imaged in the optical/NIR observations. However, the dramatic resolution difference between the sub-mm map and the optical/NIR images make it difficult to confirm this hypothesis. Aims. In a previous paper, we reported the detection of 1.4 GHz continuum radio emission coincident with this sub-mm source using VLA archival data. To fully understand the relation between this radio emission, the sub-mm emission, and the optical/IR multiplyimaged sources, we have re-observed the cluster with the VLA at higher resolution. Methods. The previous archival data has been re-reduced and combined with the new observations to produced a deep (∼10 μJy beam −1 ), high resolution (∼2 ) map centred on the cluster core. The strong lensing effect in the radio data has been quantified by constructing a new lens model of the cluster. Results. From the high resolution map we have robustly identified six radio sources located within SMM J 04542-0301. The brightest and most extended of these sources (RJ) is located in the middle of the sub-mm emission, and has no obvious counterpart in the optical/NIR. Three other detections (E1, E2 and E3) seem to be associated with the images of one of the EROs (B), although the NIR and radio emission appear to originate at slightly different positions in the source plane. The last two detections (CR1 and CR2), for which no optical/NIR counterpart have been found, seem to constitute two relatively compact emitting regions embedded in a ∼5 extended radio source located at the position of the sub-mm peak. The presence of this extended component (which contributes 38% of the total radio flux in this region) can only be explained if it is being produced by a lensed region of dust obscured star formation in the center of the merger. A comparison between the radio and sub-mm data at the same resolution suggests that E1, E2, E3, CR1 and CR2 are associated with the sub-mm emission. Conclusions. The radio observations presented in this paper provide strong observational evidence in favour of the merger hypothesis. However, the question if RJ is also contributing to the observed sub-mm emission remains open. These results illustrate the promising prospects for radio interferometry and strong gravitational lensing to study the internal structure of SMGs.

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Section: Fig 1 Summary Of the Results Presented Inmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

Alba

Koopmans²,

Garrett³

et al. 2010

A&A

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“…For comparison, an intensely star-forming HyLIRG (hyperluminous infrared galaxy) with far-infrared luminosity L FIR = 1 × 10 13 L would produce a rest-frame 1.4 GHz radio power of 10 25.0 W Hz −1 , assuming a far-infrared-to-radio luminosity ratio of 2.0, as found for high-redshift submillimeter galaxies (e.g., Vlahakis et al 2007;Seymour et al 2009; Thomson et al 2014), and a radio spectral index typical of star formation of α = −0.7 to −0.8. This is very similar to the steep spectral indices α ∼ −1.0 that are characteristic of high-redshift radio galaxies, making it even more difficult to disentangle the contribution of AGNs and star formation to lower-power radio sources than those studied here.…”

Section: Samplementioning

confidence: 99%

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Collet

Nesvadba

Breuck

et al. 2016

A&A

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Most successful galaxy formation scenarios now postulate that the intense star formation in massive, high-redshift galaxies during their major growth period was truncated when powerful AGNs launched galaxy-wide outflows of gas that removed large parts of the interstellar medium. SINFONI imaging spectroscopy of the most powerful radio galaxies at z ∼ 2 show clear signatures of such winds, but are too rare to be good representatives of a generic phase in the evolution of all massive galaxies at high redshift. Here we present SINFONI imaging spectroscopy of the rest-frame optical emission-line gas in 12 radio galaxies at redshifts ∼2. Our sample spans a range in radio power that is intermediate between the most powerful radio galaxies with known wind signatures at these redshifts and vigorous starburst galaxies, and are about two orders of magnitude more common than the most powerful radio galaxies. Thus, if AGN feedback is a generic phase of massive galaxy evolution for reasonable values of the AGN duty cycle, these are just the sources where AGN feedback should be most important. Our sources show a diverse set of gas kinematics ranging from regular velocity gradients with amplitudes of Δv = 200−400 km s −1 consistent with rotating disks to very irregular kinematics with multiple velocity jumps of a few 100 km s −1 . Line widths are generally high, typically around FWHM = 800 km s −1 , more similar to the more powerful high-z radio galaxies than mass-selected samples of massive high-z galaxies without bright AGNs, and consistent with the velocity range expected from recent hydrodynamic models. A broad Hα line in one target implies a black hole mass of a few 10 9 M . Velocity offsets of putative satellite galaxies near a few targets suggest dynamical masses of a few 10 11 M for our sources, akin to the most powerful high-z radio galaxies. Ionized gas masses are 1−2 orders of magnitude lower than in the most powerful radio galaxies, and the extinction in the gas is relatively low, up to A V ∼ 2 mag. The ratio of line widths, σ, to bulk velocity, v, is so large that even the gas in galaxies with regular velocity fields is unlikely to be gravitationally bound. It is unclear, however, whether the large line widths are due to turbulence or unresolved, local outflows as are sometimes observed at low redshifts. We compare our sources with sets of radio galaxies at low and high redshift, finding that they may have more in common with gas-rich nearby radio galaxies with similar jet power than with the most powerful high-z radio galaxies. Comparison of the kinetic energy with the energy supply from the AGNs through jet and radiation pressure suggests that the radio source still plays a dominant role for feedback, consistent with low-redshift radio-loud quasars.

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“…Therefore, a relation consistent with the local one is an indication of star formation dominating both the IR and radio emissions. There is growing evidence that the correlation holds at redshifts z 1 (Garrett 2002;Gruppioni et al 2003;Appleton et al 2004;Boyle et al 2007;Marleau et al 2007;Vlahakis et al 2007;Yang et al 2007). At higher redshifts sample sizes are small making it difficult to draw robust conclusions (Appleton et al 2004;Kovács et al 2006;Beswick et al 2008;Ibar et al 2008;Sajina et al 2008;Garn et al 2009;Murphy et al 2009;Murphy 2009;Rieke et al 2009;Seymour et al 2009;Younger et al 2009b;Sargent et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

234

278

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The nature of galaxies selected at submillimeter wavelengths (SMGs, S 850 3 mJy), some of the bolometrically most luminous objects at high redshifts, is still elusive. In particular their star formation histories and source of emission are not accurately constrained. In this paper we introduce a new approach to analyse the SMG data. Namely, we present the first self-consistent UV-to-radio spectral energy distribution fits of 76 SMGs with spectroscopic redshifts using all photometric datapoints from ultraviolet to radio simultaneously. We find that they are highly star-forming (median star formation rate 713 M yr −1 for SMGs at z > 0.5), moderately dust-obscured (median A V ∼ 2 mag), hosting significant stellar populations (median stellar mass 3.7 × 10 11 M ) of which only a minor part has been formed in the ongoing starburst episode. This implies that in the past, SMGs experienced either another starburst episode or merger with several galaxies. The properties of SMGs suggest that they are progenitors of present-day elliptical galaxies. We find that these bright SMGs contribute significantly to the cosmic star formation rate density (∼20%) and stellar mass density (∼30-50%) at redshifts 2-4. Using number counts at low fluxes we find that as much as 80% of the cosmic star formation at these redshifts took place in SMGs brighter than 0.1 mJy. We find evidence that a linear infrared-radio correlation holds for SMGs in an unchanged form up to redshift of 3.6, though its normalization is offset from the local relation by a factor of ∼2.1 towards higher radio luminosities. We present a compilation of photometry data of SMGs and determinations of cosmic SFR and stellar mass densities.

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The far-infrared-radio relationship at high and low redshift

Cited by 45 publications

References 47 publications

Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

Radio counterpart of the lensed submm emission in the cluster MS0451.6-0305: new evidence for the merger scenario

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

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