The Discovery of 1000 km s[FORMULA][F][SUP]-1[/SUP][/F][/FORMULA] Outflows in Massive Poststarburst Galaxies at [FORMULA][F]z=0.6[/F][/FORMULA]

Tremonti, Christy; Moustakas, John; Diamond‐Stanic, Aleksandar M.

doi:10.1086/520083

Cited by 341 publications

(431 citation statements)

References 34 publications

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“…While environmental quenching may be dominant for intermediate-mass QGs (Peng et al 2010), stacking analyses at radio (this work) and X-ray (Olsen et al 2013) wavelengths reveal that massive QGs harbor low-luminosity AGNs. AGNs provide a viable mechanism for quenching SF in galaxies, either through high-velocity outflows of gas (Tremonti et al 2007;Cimatti et al 2013;Cicone et al 2014), or heating up the gas to prevent star formation. This is supported by the enhanced AGN fraction among transitory objects between SFGs and QGs (e.g., Barro et al 2014).…”

Section: Discussion and Summarymentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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We performed a comprehensive stacking analysis on ∼14,200 quiescent galaxy (QG) candidates at z=0-3 across mid-, far-infrared (MIR and FIR), and radio wavelengths. Identified via their rest-frame NUV−r and r−J colors, the QG candidates (M M 10 9.8 12.2 - =  ) have drastically different IR and radio properties depending on their 24 μm emission strength. The fraction of QG candidates with strong 24 μm emission (equivalent to inferred star formation rates SFR M yr 100, hereafter "IR-bright") increases with redshift and peaks at 15%, and their stacked MIPS 24 μm, Herschel (PACS and SPIRE) and VLA emissions are consistent with being starforming galaxies (SFGs). In contrast, the majority of QG candidates are faint or undetected at 24 μm individually (i.e., SFR 24 <100 M e yr −1 , hereafter "IR-faint"). Their low dust-obscured SFRs derived from Herschel stacking (SFR H  3, 15, 50 M e yr −1 out to z∼1, 2, 3) are >2.5-12.5×lower than compared to SFGs. This is consistent with the quiescence, as expected from their low unobscured SFRs, as inferred from modeling their ultraviolet-to-NIR photometry. The discrepancy between the L IR derived from stacking Herschel and 24 μm indicates that IRfaint QGs have dust SEDs that are different from those of SFGs. For the most massive (M M 10 11    ) IR-faint QGs at z<1.5, the stacked 1.4 GHz emission is in excess of that expected from other SFR indicators, suggesting a widespread presence of low-luminosity active galactic nuclei. Our results reaffirm the existence of a significant population of QGs out to z=3, thus corroborating the need to quench star formation in galaxies at early epochs.

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Section: Discussion and Summarymentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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“…Some of the most successful models assume that a significant amount of the rest-mass energy of the matter accreted by the black hole is available to drive a powerful galactic wind (e.g., Hopkins et al 2008;Di Matteo et al 2008). To date, there is little strong evidence in the local universe that such processes operate on galactic scales in typical Seyfert galaxies, although some spectacular outflows (likely to have been launched by a previous AGN outburst) have been observed in massive post-starburst systems at intermediate redshifts (Tremonti et al 2007).…”

Section: T M Heckmanmentioning

confidence: 99%

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Heckman

2009

Proc. IAU

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Abstract. I begin by summarizing the evidence that there is a close relationship between the evolution of galaxies and supermassive black holes. They evidently share a common fuel source, and feedback from the black hole may be needed to suppress over-cooling in massive galaxies.I then review what we know about the co-evolution of galaxies and black holes in the modern universe (z < 1). We now have a good documentation of which black holes are growing (the lower mass ones), where they are growing (in the less massive early-type galaxies), and how this growth is related in a statistical sense to star formation in the central region of the galaxy. The opportunity in the next decade will be to use the new observatories to undertake ambitious programs of 3-D imaging spectroscopy of the stars and gas in order to understand the actual astrophysical processes that produce the demographics we observe. At high redshift (z > 2), the most massive black holes and the progenitors of the most massive galaxies are forming. Here, we currently have a tantalizing but fragmented view of their co-evolution. In the next decade, the huge increase in sensitivity and discovery power of our observatories will enable us to analyze the large, complete samples we need to achieve robust and clear results.

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“…The outflow can transport energy, momentum, mass, heavy elements from the accretion disc and/or the vicinity of central region to the host galaxy and IGM, which regulate the efficiency of accretion onto the central supermassive black hole (e.g., Emmering et al 1992;Konigl & Kartje 1994), and influence the evolution of the host galaxy and surrounding environment (e.g., Tremonti et al 2007;Cattaneo et al 2009;Yuan & Narayan 2014;Ishibashi & Fabian 2014). Intrinsic absorption lines, including BALs, mini-BALs and NALs, are often utilized to study properties of the quasar outflow.…”

Section: Introductionmentioning

confidence: 99%

Narrow absorption lines with two observations from the Sloan Digital Sky Survey

Chen¹,

Gu²,

Chen³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We assemble 3524 quasars from Sloan Digital Sky Survey (SDSS) with repeated observations to search for variations of narrow C IVλλ1548, 1551 and Mg IIλλ2796, 2803 absorption doublets in spectral regions shortward of 7000Å at the observed frame, which corresponds to time-scales of about 150 ∼ 2643 days at quasar rest frame. In these quasar spectra, we detect 3580 C IV absorption systems with z abs = 1.5188 ∼ 3.5212, and 1809 Mg II absorption systems with z abs = 0.3948 ∼ 1.7167. In term of the absorber velocity (β) distribution at quasar rest frame, we find a substantial number of C IV absorbers with β < 0.06, which might be connected to the absorptions of quasar outflows. The outflow absorptions peak at υ ≈ 2000 km s −1 and drop rapidly below the peak value. Among 3580 C IV absorption systems, 52 systems (∼ 1.5%) show obvious variations in equivalent widths at the absorber rest frame (W r ): 16 enhanced, 16 emerged, 12 weaken, and 8 disappeared systems, respectively. We find that changes in W r λ1548 are neither related to time-scales of the two SDSS observations, nor to absorber velocities at the quasar rest frame. Variable absorptions in low-ionization species are important to constraint the physical conditions of absorbing gas. There are two variable Mg II absorption systems measured from SDSS spectra detected by Hacker et al. However, in our Mg II absorption sample, we find that neither shows variable absorption with confident levels of > 4σ for λ2796 lines and > 3σ for λ2803 lines.

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The Discovery of 1000 km s[FORMULA][F][SUP]-1[/SUP][/F][/FORMULA] Outflows in Massive Poststarburst Galaxies at [FORMULA][F]z=0.6[/F][/FORMULA]

Cited by 341 publications

References 34 publications

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

The Co-Evolution of Galaxies and Black Holes: Current Status and Future Prospects

Narrow absorption lines with two observations from the Sloan Digital Sky Survey

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