VERTICO II: How H i-identified Environmental Mechanisms Affect the Molecular Gas in Cluster Galaxies

Zabel, Nikki; Brown, Toby; Wilson, C. D.; Davis, Timothy A.; Cortese, Luca; Parker, Laura C.; Boselli, A.; Catinella, Barbara; Chown, R.; Chung, Aeree; Deb, Tirna; Ellison, Sara L.; Jiménez-Donaire, María J.; Lee, Bumhyun; Roberts, Ian; Spekkens, Kristine; Stevens, Adam; Thorp, Mallory; Tonnesen, Stephanie; Villanueva, V.

doi:10.3847/1538-4357/ac6e68

Cited by 29 publications

(53 citation statements)

References 102 publications

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“…Figure 4 shows the molecular gas radial profiles derived in this work (blue-solid line), and their ±1σ uncertainties (blue-shaded areas) for the 38 VERTICO galaxies selected here. Although radial profiles in Brown et al (2021) and used in Zabel et al (2022) are not corrected for inclination, they agree fairly with those included in Figure 4 (particularly at r < 0.3r 25 ) when we multiply them by cos(i). Annuli are centered on the optical galaxy position and aligned with the major-axis position angle, taken from Table 1 in Brown et al (2021).…”

Section: Co Radial Profilessupporting

confidence: 61%

“…Recent observational evidence has shown that molecular gas content and its distribution in the disk of cluster galaxies depends on the effect of the environment on the HI distribution (e.g., Chung & Kim 2014;Boselli et al 2014;Cortese et al 2021;Zabel et al 2022). In order to characterize the behavior of the molecular gas as a function of the cluster environmental effects on the atomic gas, we use the HI classification from Yoon et al (2017) (hereafter HI-Class).…”

Section: Basic Equations and Assumptionsmentioning

confidence: 99%

“…As discussed in §3.1, we derive the molecular gas radial profiles by measuring the averaged azimuthal CO surface density, after performing a spectral stacking, in elliptical annuli in the 9 CO(2-1) datacubes. Although CO radial profiles for VERTICO galaxies are already presented in Brown et al (2021) and Zabel et al (2022) (both using the same methodology described in §4.3 of Brown et al 2021), the CO spectral stacking expands the radial coverage and recovers faint CO emission especially in the outermost regions of most cases. Figure 4 shows the molecular gas radial profiles derived in this work (blue-solid line), and their ±1σ uncertainties (blue-shaded areas) for the 38 VERTICO galaxies selected here.…”

Section: Co Radial Profilesmentioning

confidence: 99%

“…Cluster galaxies typically contain less atomic gas than their field counterparts, and commonly show signs of truncation and perturbed HI morphologies (e.g., Haynes & Giovanelli 1984;Chung et al 2009;Yoon et al 2017;Brown et al 2017;Stevens & Brown 2017;Watts et al 2020a,b;Molnár et al 2022). Although the molecular gas is closer to galaxy centers and more tightly bound than the HI (Davis et al 2013), several studies show that the H 2 is also susceptible to significant variations due to environmental effects (e.g., Fumagalli et al 2009;Boselli et al 2014;Lee et al 2017;Lee & Chung 2018;Zabel et al 2019;Lizée et al 2021;Stevens et al 2021;Brown et al 2021;Zabel et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…Although using a small sample of galaxies with an heterogeneous set of molecular gas data, Boselli et al (2014) find a mild statistically significant correlation between the H 2 and HI deficiencies in Virgo galaxies from the Herschel Reference Survey (HRS; Boselli et al 2010), supporting the hypothesis that they are simultaneously affected. Zabel et al (2022) note that VERTICO galaxies with larger HI deficiencies (an indicator of how poor in HI individual galaxies are when compared to field galaxies of the same size and morphological type, Haynes & Giovanelli 1984;Warmels 1986;Cayatte et al 1990; see also Cortese et al 2021 for a detailed description) also have more compact and steeper H 2 radial profiles. Although with significantly different physical properties than the Virgo cluster, Loni et al (2021) find however a significant scatter in the global molecular-to-atomic ratios, R mol , in galaxies selected from the Fornax cluster, which suggests that the effects of environmental mechanisms on the atomicto-molecular gas transition may not be straightforward (e.g., Stevens et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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VERTICO IV: Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals

Villanueva¹,

Bolatto²,

Vogel³

et al. 2022

Preprint

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We measure the molecular-to-atomic gas ratio, R mol , and the star formation rate (SFR) per unit molecular gas mass, SFE mol , in 38 nearby galaxies selected from the Virgo Environment Traced in CO (VERTICO) survey. We stack ALMA 12 CO(J=2-1) spectra coherently using HI velocities from the VIVA survey to detect faint CO emission out to galactocentric radii r gal ∼ 1.2 r 25 . We determine their scale-lengths for the molecular and stellar components and find a roughly 3:5 ratio between them compared to ∼ 1:1 in field galaxies, indicating that the CO emission is more centrally concentrated than the stars. We compute R mol as a function of different physical quantities. While the spatiallyresolved R mol on average decreases with increasing radius, we find that the mean molecular-to-atomic gas ratio within the stellar effective radius R e , R mol (r < R e ), shows a systematic increase with the level of HI, truncation and/or asymmetry (HI perturbation). Analysis of the molecular-and the atomic-to-stellar mass ratios within R e , R mol (r < R e ) and R atom (r < R e ), shows that VERTICO galaxies have increasingly lower R atom (r < R e ) for larger levels of H I perturbation (compared to field galaxies matched in stellar mass), but no significant change in R mol (r < R e ). We also measure a clear systematic decrease of the SFE mol within R e , SFE mol (r < R e ), with increasingly perturbed HI. Therefore, compared to galaxies from the field, VERTICO galaxies are more compact in CO emission

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Section: Co Radial Profilessupporting

confidence: 61%

Section: Basic Equations and Assumptionsmentioning

confidence: 99%

Section: Co Radial Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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VERTICO IV: Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals

Villanueva¹,

Bolatto²,

Vogel³

et al. 2022

Preprint

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The ALMaQUEST Survey XV: The dependence of the molecular-to-atomic gas ratios on resolved optical diagnostics

Yu,

Zheng,

Tsai

et al. 2024

Sci. China Phys. Mech. Astron.

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VERTICO V: The environmentally driven evolution of the inner cold gas discs of Virgo cluster galaxies

Watts

Cortese

Thorp

et al. 2023

Publ. Astron. Soc. Aust.

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The quenching of cluster satellite galaxies is inextricably linked to the suppression of their cold interstellar medium (ISM) by environmental mechanisms. While the removal of neutral atomic hydrogen (H i) at large radii is well studied, how the environment impacts the remaining gas in the centres of galaxies, which are dominated by molecular gas, is less clear. Using new observations from the Virgo Environment traced in CO survey (VERTICO) and archival H i data, we study the H i and molecular gas within the optical discs of Virgo cluster galaxies on 1.2-kpc scales with spatially resolved scaling relations between stellar ( $\Sigma_{\star}$ ), H i ( $\Sigma_{\text{H}\,{\small\text{I}}}$ ), and molecular gas ( $\Sigma_{\text{mol}}$ ) surface densities. Adopting H i deficiency as a measure of environmental impact, we find evidence that, in addition to removing the H i at large radii, the cluster processes also lower the average $\Sigma_{\text{H}\,{\small\text{I}}}$ of the remaining gas even in the central $1.2\,$ kpc. The impact on molecular gas is comparatively weaker than on the H i, and we show that the lower $\Sigma_{\text{mol}}$ gas is removed first. In the most H i-deficient galaxies, however, we find evidence that environmental processes reduce the typical $\Sigma_{\text{mol}}$ of the remaining gas by nearly a factor of 3. We find no evidence for environment-driven elevation of $\Sigma_{\text{H}\,{\small\text{I}}}$ or $\Sigma_{\text{mol}}$ in H i-deficient galaxies. Using the ratio of $\Sigma_{\text{mol}}$ -to- $\Sigma_{\text{H}\,{\small\text{I}}}$ in individual regions, we show that changes in the ISM physical conditions, estimated using the total gas surface density and midplane hydrostatic pressure, cannot explain the observed reduction in molecular gas content. Instead, we suggest that direct stripping of the molecular gas is required to explain our results.

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VERTICO II: How H i-identified Environmental Mechanisms Affect the Molecular Gas in Cluster Galaxies

Cited by 29 publications

References 102 publications

VERTICO IV: Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals

VERTICO IV: Environmental Effects on the Gas Distribution and Star Formation Efficiency of Virgo Cluster Spirals

The ALMaQUEST Survey XV: The dependence of the molecular-to-atomic gas ratios on resolved optical diagnostics

VERTICO V: The environmentally driven evolution of the inner cold gas discs of Virgo cluster galaxies

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