Evidence for galaxy quenching in the green valley caused by a lack of a circumgalactic medium

Kacprzak, Glenn G.; Nielsen, Nikole M.; Nateghi, Hasti; Churchill, Christopher W.; Pointon, Stephanie K.; Nanayakkara, Themiya; Muzahid, Sowgat; Charlton, Jane C.

doi:10.1093/mnras/staa3461

Cited by 11 publications

(9 citation statements)

References 118 publications

(195 reference statements)

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“…While it is unclear what causes the abnormal CGM composition in M 100, the Virgo cluster environment likely contributed significantly. Interestingly, the non-existence of a cool CGM has also been reported recently by Kacprzak et al (2021) in a higher redshift field galaxy. These authors claim that the loss of the cool CGM is causing that galaxy to turn "green" and will eventually lead to the quenching of star formation altogether.…”

Section: The Fate Of Ahcs and Their Connection To The Cgmsupporting

confidence: 73%

DIISC-I: The Discovery of Kinematically Anomalous HI Clouds in M 100

Gim,

Borthakur,

Momjian

et al. 2021

Preprint

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We report the discovery of two kinematically anomalous atomic hydrogen (HI) clouds in M 100 (NGC 4321), which was observed as part of the Deciphering the Interplay between the Interstellar medium, Stars, and the Circumgalactic medium (DIISC) survey in HI 21 cm at 3.3 km s −1 spectroscopic and 44 ×30 spatial resolution using the Karl G. Jansky Very Large Array a) . These clouds were identified as structures that show significant kinematic offsets from the rotating disk of M100. The velocity offsets of 40 km s −1 observed in these clouds are comparable to the offsets seen in intermediatevelocity clouds (IVCs) in the circumgalactic medium (CGM) of the Milky Way and nearby galaxies. We find that one anomalous cloud in M 100 is associated with star-forming regions detected in Hα and far-ultraviolet imaging. Our investigation shows that anomalous clouds in M 100 may originate from multiple mechanisms, such as star formation feedback-driven outflows, ram-pressure stripping, and tidal interactions with satellite galaxies. Moreover, we do not detect any cool CGM at 38.8 kpc from the center of M 100, giving an upper limit of N(HI) ≤ 1.7×10 13 cm −2 (3σ). Since M 100 is in the Virgo cluster, the non-existence of neutral/cool CGM is a likely pathway for turning it into a red galaxy.

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Section: The Fate Of Ahcs and Their Connection To The Cgmsupporting

confidence: 73%

DIISC-I: The Discovery of Kinematically Anomalous HI Clouds in M 100

Gim,

Borthakur,

Momjian

et al. 2021

Preprint

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“…As the chemical evolution proceeds, the iron content of the ISM increases and its [Mg/Fe] abundance ratio decreases, producing 8 Other quenching mechanisms have been proposed, such as e.g. a drastic drop of the gas accretion, caused by a switch from cold-flow mode to hot mode (Noguchi 2018), a massive merger, heating the halo gas and inhibiting its accretion (Vincenzo et al 2019) or a depletion of the circumgalactic medium (Kacprzak et al 2020). 9 magnesium and iron being diluted in similar proportions, the [Mg/Fe] abundance ratio is not significantly modified.…”

Section: Formation Of the Galactic Disc: The Haywood Et Al Scenariomentioning

confidence: 99%

Radial structure and formation of the Milky Way disc

Katz

Gómez

Haywood

et al. 2021

A&A

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Context. The formation of the Galactic disc is an enthusiastically debated issue. Numerous studies and models seek to identify the dominant physical process(es) that shaped its observed properties; for example, satellite accretion, starburst, quenching, gas infall, and stellar radial migration. Aims. Taking advantage of the improved coverage of the inner Milky Way provided by the SDSS DR16 APOGEE catalogue and of the ages published in the APOGEE-AstroNN Value Added Catalogue (VAC), we examined the radial evolution of the chemical and age properties of the Galactic stellar disc with the aim of better constraining its formation. Methods. Using a sample of 199 307 giant stars with precise APOGEE abundances and APOGEE-AstroNN ages, selected in a ±2 kpc layer around the galactic plane, we assessed the dependency as a function of guiding radius of (i) the median metallicity, (ii) the ridge lines of the [Fe/H] − [Mg/Fe] and age–[Mg/Fe] distributions, and (iii) the age distribution function (ADF). Results. The giant star sample allows us to probe the radial behaviour of the Galactic disc from Rg = 0 to 14−16 kpc. The thick disc [Fe/H] − [Mg/Fe] ridge lines follow closely grouped parallel paths, supporting the idea that the thick disc did form from a well-mixed medium. However, the ridge lines present a small drift in [Mg/Fe], which decreases with increasing guiding radius. At sub-solar metallicity, the intermediate and outer thin disc [Fe/H] − [Mg/Fe] ridge lines follow parallel sequences shifted to lower metallicity as the guiding radius increases. We interpret this pattern as the signature of a dilution of the interstellar medium from Rg ∼ 6 kpc to the outskirts of the disc, which occurred before the onset of the thin disc formation. The APOGEE-AstroNN VAC provides stellar ages for statistically significant samples of thin disc stars from the Galactic centre up to Rg ∼ 14 kpc. An important result provided by this dataset is that the thin disc presents evidence of an inside-out formation up to Rg ∼ 10 − 12 kpc. Moreover, about ∼7 Gyr ago, the [Mg/Fe] ratio in the outer thin disc (Rg > 10 kpc) was higher by about ∼0.03−0.05 dex than in the more internal regions of the thin disc. This could be the fossil record of a pollution of the outer disc gas reservoir by the thick disc during its starburst phase.

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“…This phenomena might be related to the inability for galaxies in groups to continue the gas accretion necessary to fuel star formation. This has been observed in galaxy clusters (Yoon & Putman 2013;Gim et al 2021), and when scaled to the group environment, could indicate the beginning of the preprocessing and quenching processes (Zabludoff & Mulchaey 1998;McGee et al 2009;Wetzel et al 2013;Schawinski et al 2014;Crossett et al 2017;Kacprzak et al 2021).…”

Section: H I Lyα Absorptionmentioning

confidence: 67%

Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

McCabe,

Borthakur,

Heckman

et al. 2021

Preprint

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We present the results of the COS Intragroup Medium (COS-IGrM) Survey that used the Cosmic Origins Spectrograph on the Hubble Space Telescope to observe a sample of 18 UV bright quasars, each probing the intragroup medium (IGrM) of a galaxy group. We detect Lyα, C II, N V, Si II, Si III, and O VI in multiple sightlines. The highest ionization species detected in our data is O VI, which was detected in 8 out of 18 quasar sightlines. The wide range of ionization states observed provide evidence that the IGrM is patchy and multiphase. We find that the O VI detections generally align with radiatively cooling gas between 10 5.8 and 10 6 K. The lack of O VI detections in 10 of the 18 groups illustrates that O VI may not be the ideal tracer of the volume filling component of the IGrM. Instead, it either exists at trace levels in a hot IGrM or is generated in the boundary between the hotter IGrM and cooler gas.

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Evidence for galaxy quenching in the green valley caused by a lack of a circumgalactic medium

Cited by 11 publications

References 118 publications

DIISC-I: The Discovery of Kinematically Anomalous HI Clouds in M 100

DIISC-I: The Discovery of Kinematically Anomalous HI Clouds in M 100

Radial structure and formation of the Milky Way disc

Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

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