Amblard et al. Reply:

Amblard, François; Maggs, A. C.; Yurke, Bernard; Pargellis, A. N.; Leibler, Stanislas

doi:10.1103/physrevlett.81.1135

Cited by 91 publications

(150 citation statements)

References 4 publications

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“…Excluding the sources where T was fixed, we found a median dust temperature across the whole sample of 26 K with a standard deviation of 8 K (or 23 ± 7 K for β = 2). This result closely agrees with the rest-frame dust temperatures determined for BLAST sources measured by Dye et al (2009) as well as those of the sample of H-ATLAS galaxies studied in Amblard et al (2010; see also other temperature comparisons therein).…”

Section: Sed Fittingsupporting

confidence: 80%

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Dye

Dunne

Eales

et al. 2010

A&A

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We have determined the luminosity function of 250 μm-selected galaxies detected in the ∼14 deg 2 science demonstration region of the Herschel-ATLAS project out to a redshift of z = 0.5. Our findings very clearly show that the luminosity function evolves steadily out to this redshift. By selecting a sub-group of sources within a fixed luminosity interval where incompleteness effects are minimal, we have measured a smooth increase in the comoving 250 μm luminosity density out to z = 0.2 where it is 3.6 +1.4 −0.9 times higher than the local value.

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Section: Sed Fittingsupporting

confidence: 80%

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Dye

Dunne

Eales

et al. 2010

A&A

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“…6, we compare the FIR colours of the detected AGN sub-sample and the stacked values of the total sub-samples (large symbols) to the FIR colours of 10 6 randomly generated modified black-body, single dust temperature T d spectra models, with a frequency dependence of ǫν ∝ ν β . In generating these models, we follow the method of Amblard et al (2010) considering uniformly distributed dust temperatures from 10 to 60 K, emissivity parameter 0 < β < 2 and redshift range similar to our sample (0.9 < z < 1.1). In order to consider for flux uncertainties in the colour-colour diagram, we have broadened the SED tracks by S (mJy) Figure 5.…”

Section: The Fir Colours Of Rlqs Rqqs and Rgsmentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1 which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that: 1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, 2) the RLQs show a SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radio AGN triggering are linked to star-formation triggering and 3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power.

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“…We set no prior on the amplitude of the modified blackbodies or each unknown image background. A hard prior, T > 10 K, is motivated by the fact that neither Dale et al (2012) nor Amblard et al (2010) found any colder Herschel galaxies in either the nearby or distant Universe, respectively. While we have corrected the relative pointing of Herschel and HST, we are unable to find any significant pointing shift in the JCMT due to the lower signal-to-noise in the map than what is available in the Herschel SPIRE observations.…”

Section: Model Fittingmentioning

confidence: 99%

Disentangling a group of lensed submm galaxies at z∼ 2.9

Mackenzie¹,

Scott²,

Smail³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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MS 0451.6−0305 is a rich galaxy cluster whose strong lensing is particularly prominent at submm wavelengths. We combine new SCUBA-2 data with imaging from Herschel SPIRE and PACS and HST in order to try to understand the nature of the sources being lensed. In the region of the "giant submm arc," we uncover seven multiply imaged galaxies (up from the previously known three), of which six are found to be at a redshift of z ∼ 2.9, and possibly constitute an interacting system. Using a novel forward-modelling approach, we are able to simultaneously deblend and fit SEDs to the individual galaxies that contribute to the giant submm arc, constraining their dust temperatures, far infrared luminosities and star formation rates. The submm arc first identified by SCUBA can now be seen to be composed of at least five distinct sources, four of these within the galaxy group at z ∼ 2.9. The total unlensed luminosity for this galaxy group is (3.1 ± 0.3) × 10 12 L , which gives an unlensed star formation rate of (450 ± 50) M yr −1 . From the properties of this system, we see no evidence of evolution towards lower temperatures in the dust temperature versus far-infrared luminosity relation for high redshift galaxies.

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Amblard et al. Reply:

Cited by 91 publications

References 4 publications

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Disentangling a group of lensed submm galaxies at z∼ 2.9

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