[논문]STAR FORMATION ACTIVITY OF GALAXIES UNDERGOING RAM PRESSURE STRIPPING IN THE VIRGO CLUSTER

Mun, Jae Yeon; Hwang, Ho Seong; Lee, Myung Gyoon; Chung, Aeree; Yoon, Hyein; Lee, Jong Chul

doi:10.5303/jkas.2021.54.1.17

STAR FORMATION ACTIVITY OF GALAXIES UNDERGOING RAM PRESSURE STRIPPING IN THE VIRGO CLUSTER 원문보기

Journal of the Korean astronomical society = 천문학회지, v.54 no.1, 2021년, pp.17 - 35

Mun, Jae Yeon (Department of Physics and Astronomy, Seoul National University) , Hwang, Ho Seong (Korea Astronomy and Space Science Institute) , Lee, Myung Gyoon (Department of Physics and Astronomy, Seoul National University) , Chung, Aeree (Department of Astronomy, Yonsei University) , Yoon, Hyein (Department of Astronomy, Yonsei University) , Lee, Jong Chul (Korea Astronomy and Space Science Institute)

Abstract ▼ AI-Helper

We study galaxies undergoing ram pressure stripping in the Virgo cluster to examine whether we can identify any discernible trend in their star formation activity. We first use 48 galaxies undergoing different stages of stripping based on H i morphology, H i deficiency, and relative extent to the stellar disk, from the VIVA survey. We then employ a new scheme for galaxy classification which combines H i mass fractions and locations in projected phase space, resulting in a new sample of 365 galaxies. We utilize a variety of star formation tracers, which include g - r, WISE [3.4]-[12] colors, and starburstiness that are defined by stellar mass and star formation rates to compare the star formation activity of galaxies at different stripping stages. We find no clear evidence for enhancement in the integrated star formation activity of galaxies undergoing early to active stripping. We are instead able to capture the overall quenching of star formation activity with increasing degree of ram pressure stripping, in agreement with previous studies. Our results suggest that if there is any ram pressure stripping induced enhancement, it is at best locally modest, and galaxies undergoing enhancement make up a small fraction of the total sample. Our results also indicate that it is possible to trace galaxies at different stages of stripping with the combination of H i gas content and location in projected phase space, which can be extended to other galaxy clusters that lack high-resolution H i imaging.

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표/그림 (11)

그림 Figure 1. Comparison diagrams of stellar masses measured via an SED fit of EVCC ugriz photometry with Le Phare (left), and of star formation rates derived using total IR luminosities with those given in the SDSS MPA/JHU DR7 VAGC (right). The dashed lines in the top panels show the one-to-one relations.
표 Table 1 The VIVA sample defined by different stages of gas stripping
그림 Figure 2. Left: Projected phase-space diagram with regions A to E defined according to time since infall into the cluster center, closely following the classification in Rhee et al. (2017). Clustercentric distance and velocity are normalized by the cluster virial radius r₂₀₀ and cluster velocity dispersion σ_cl, respectively. First infallers are located in Region A, recent infallers in Region B, intermediate infallers in Region C, and ancient infallers in Region D. Region E is defined by field galaxies. Right: Projected phase-space diagram of RPS class galaxies and the rest of the EVCC sample shown as reference (grey open symbols).
그림 Figure 3. Total IR-derived star formation rates, optical, and mid-infrared colors (from top to bottom) as a function of stellar mass for Virgo galaxies with defined RPS classes from Yoon et al. (2017) and the remaining EVCC galaxies with no defined classes plotted as reference. The solid black lines dene a reference sequence for each star formation activity tracer, to normalize for the effects of different masses. The reference sequence for SFR_IR is the star-forming main sequence defined by Elbaz et al. (2007), and the dashed lines are the lower and upper bounds to the fit. The solid line in the middle panel is the red sequence, which was derived based on a best linear t of non-RPS Class galaxies with M_* > 1.5×10¹⁰ M_⊙ and g − r > 0.58. The solid line in the bottom panel is adopted from the peak of the mid-infrared color distribution of star-forming galaxies in Hwang et al. (2012b).
그림 Figure 4. Starburstiness (R_SB), Δ(g − r), and Δ([3.4] − [12]) histograms (from left to right). Vertical lines denote the locus of the reference sequence (i.e., star-forming main sequence for R_SB, red sequence for g − r, star-forming sequence for [3.4] − [12]). Certain members, for which cluster membership is given by the EVCC, with no defined RPS classifications are plotted together for reference. The arrows represent the median values for each sample. Bin counts were increased by a factor of 5 (10 for the Δ(g − r) distribution) for RPS galaxies for a fair comparison with the reference sample. The scale of the original bin counts are labeled on the right hand side of each panel. The representative (either the mean or the median) errors for each parameter are shown in the top right corner of each panel.
$Figure 5. Left: H I mass fraction as a function of stellar mass, for which each of the shaded regions mark the range of H I mass fractions of each group, as defined by Equations (2)−(4). The blue line is the reference sequence as defined by a best linear fit of Class 0 and I galaxies, defined by Equation (1). Right: H I mass fraction as a function of stellar mass for the RPS class sample, to verify whether the selected ranges of Δ(logMHI=M*) for each group are consistent with those of the RPS class sample.$ 그림 Figure 5. Left: H _I mass fraction as a function of stellar mass, for which each of the shaded regions mark the range of H _I mass fractions of each group, as defined by Equations (2)−(4). The blue line is the reference sequence as defined by a best linear fit of Class 0 and I galaxies, defined by Equation (1). Right: H _I mass fraction as a function of stellar mass for the RPS class sample, to verify whether the selected ranges of Δ(logM_HI=M_*) for each group are consistent with those of the RPS class sample.
그림 Figure 6. Δ(log M_HI=M_*) histogram with the resulting Gaussian Mixture Model (GMM) overlaid on top. Each Gaussian component specifies the mean and range of a potential H _I group. The blue component represents the H _I-normal to rich galaxies, the green represents the H _I-poorish galaxies, and the red the H _I-poor. The grey dashed lines mark the intersections between the different Gaussian components.
그림 Figure 7. Projected phasespace diagram of all newly defined H _I stripping groups. The black solid lines indicate the boundaries between different regions of time since infall as shown in Figure 2. The final group candidates are shown as filled color symbols, whereas those that did not satisfy the condition of expected location in phase space are shown as open symbols. Red open symbols (H _I-poor galaxies located outside of Regions B through D) residing in the region defined by grey solid lines are selected as potential backsplashing candidates, which are discussed briefly in Section 4.2.2.
표 Table 2 Categorization of the EVCC into H _I stripping groups
그림 Figure 8. Star formation rates derived from total IR luminosities, optical, and mid-infrared colors (from top to bottom) as a function of stellar mass for the EVCC sample with newly defined H _I stripping groups. The reference sequences shown here are identical to the ones used in Figure 3.
그림 Figure 9. Starburstiness (R_SB), Δ(g − r), and Δ([3.4] − [12]) histograms (from left to right) for new H _I stripping groups. The downward arrows mark the median of each distribution. The vertical lines here are the same as in Figure 4. Stellar mass ranges of the subsamples used are displayed in the middle panel of each histogram. Additionally, we show the distribution of potential backsplashing candidates in the bottom panel.

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