MASSIVE MOLECULAR OUTFLOWS AND NEGATIVE FEEDBACK IN ULIRGs OBSERVED BY
                    <i>HERSCHEL</i>
                    -PACS

Sturm, E.; González-Alfonso, E.; Veilleux, Sylvain; Fischer, J.; Graciá-Carpio, J.; Hailey-Dunsheath, S.; Contursi, A.; Poglitsch, A.; Sternberg, A.; Davies, R. I.; Genzel, R.; Lutz, D.; Tacconi, L. J.; Verma, Aprajita; Maiolino, R.; Jong, J.A. de

doi:10.1088/2041-8205/733/1/l16

Cited by 554 publications

(702 citation statements)

References 38 publications

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“…Observations with PACS for the 43 ULIRGs were split between the HERUS program Spoon et al 2013) and the SHINING program Sturm et al 2011;Hailey-Dunsheath et al 2012a;González-Alfonso et al 2013;Mashian et al 2015). A similar study of the intermediate redshift ULIRG population (0.21<z<0.88) was presented by Rigopoulou et al (2014) and Magdis et al (2014).…”

Section: Observationsmentioning

confidence: 98%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

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We present the Herschel SPIRE Fourier Transform Spectroscopy (FTS) atlas for a complete flux-limited sample of local ultraluminous infrared galaxies (ULIRGs) as part of the HERschel Ultra Luminous InfraRed Galaxy Survey (HERUS). The data reduction is described in detail and was optimized for faint FTS sources ,with particular care being taken for the subtraction of the background, which dominates the continuum shape of the spectra. To improve the final spectra, special treatment in the data reduction has been given to any observation suffering from artifacts in the data caused by anomalous instrumental effects. Complete spectra are shown covering 200-671 μm, with photometry in the SPIRE bands at 250, 350, and 500 μm. The spectra include near complete CO ladders for over half of our sample, as well as fine structure lines from [C I] 370 μm, [C I] 609 μm, and [N II] 205 μm. We also detect H 2 O lines in several objects. We construct CO spectral line energy distributions (SLEDs) for the sample, and compare their slopes with the far-infrared (FIR) colors and luminosities. We show that the CO SLEDs of ULIRGs can be broadly grouped into three classes based on their excitation. We find that the mid-J (5<J<8) lines are better correlated with the total FIR luminosity, suggesting that the warm gas component is closely linked to recent star formation. The higher J transitions do not linearly correlate with the FIR luminosity, consistent with them originating in hotter, denser gas that is unconnected to the current star formation. We conclude that in most cases more than one temperature component is required to model the CO SLEDs.

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Section: Observationsmentioning

confidence: 98%

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Pearson¹,

Rigopoulou²,

Hurley³

et al. 2016

ApJS

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“…Winds are also seen in Seyfert galaxies (e.g. Tombesi et al 2011Tombesi et al , 2013Pounds & King 2013;Pounds 2014), in which velocity probably depends on the distance from the central BHs on ∼pc to ∼kpc scales (Tombesi et al 2013), and in other ultraluminous infrared galaxies with velocities depending not on star formation rate but on AGN luminosity (Sturm et al 2011). At high redshifts, AGN-hosting galaxies also show evidence of outflows (e.g.…”

Section: Introductionmentioning

confidence: 98%

Quantifying AGN-driven metal-enhanced outflows in chemodynamical simulations

Taylor

Kobayashi

2015

Monthly Notices of the Royal Astronomical Society: Letters

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“…Quasar-mode feedback occurs as a result of mergers and drives cold gas into the central regions of the galaxy. This causes rapid growth of the black hole and high accretion disc luminosities (Kauffmann & Haehnelt, 2000;Di Matteo et al, 2005), as well as massive outflows of gas (Sturm et al, 2011;Cicone et al, 2014). After this phase, radio-mode feedback begins where gas from the hot halo is fed into the black hole inefficiently, producing a jet which heats the surrounding gaseous atmosphere (Page et al, 2012;Gaspari et al, 2012;Dubois et al, 2013;Man et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

The diversity of growth histories of Milky Way-mass galaxies

Terrazas

Bell

Henriques

et al. 2016

Mon. Not. R. Astron. Soc.

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We use the semi-analytic model developed by Henriques et al. (2015) to explore the origin of star formation history diversity for galaxies that lie at the centre of their dark matter haloes and have present-day stellar masses in the range 5 − 8 × 10 10 M , similar to that of the Milky Way. In this model, quenching is the dominant physical mechanism for introducing scatter in the growth histories of these galaxies. We find that present-day quiescent galaxies have a larger variety of growth histories than starformers since they underwent 'staggered quenching' -a term describing the correlation between the time of quenching and present-day halo mass. While halo mass correlates broadly with quiescence, we find that quiescence is primarily a function of black hole mass, where galaxies quench when heating from their active galactic nuclei becomes sufficient to offset the redshift-dependent cooling rate. In this model, the emergence of a prominent quiescent population is the main process that flattens the stellar masshalo mass relation at mass scales at or above that of the Milky Way.

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MASSIVE MOLECULAR OUTFLOWS AND NEGATIVE FEEDBACK IN ULIRGs OBSERVED BY HERSCHEL -PACS

Cited by 554 publications

References 38 publications

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs

Quantifying AGN-driven metal-enhanced outflows in chemodynamical simulations

The diversity of growth histories of Milky Way-mass galaxies

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