Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping

Lee, Jeong‐Hwan; Lee, Myung Gyoon; Mun, Jae Yeon; Cho, Brian S.; Kang, Jisu

doi:10.3847/2041-8213/ac6e39

Cited by 13 publications

(13 citation statements)

References 46 publications

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“…Third, the star formation activity of jellyfish galaxies tends to increase as galaxy stellar mass increases, as shown in Figure 12. This reflects the SFR-mass relation of jellyfish galaxies as also shown in Figures 2 and 4 in Lee et al (2022). Finally, the star formation activity of jellyfish galaxies tends to increase as the host cluster velocity dispersion increases, as shown in Figure 13.…”

Section: Phase-space Of the Jellyfish Galaxiessupporting

confidence: 59%

“…Finally, the star formation activity of jellyfish galaxies tends to increase as the host cluster velocity dispersion increases, as shown in Figure 13. In this context, Lee et al (2022) revealed that jellyfish galaxies with strong RPS signatures show more enhanced star formation activity in more massive clusters with a higher degree of RPS.…”

Section: Phase-space Of the Jellyfish Galaxiesmentioning

confidence: 98%

“…In addition, the median SFR fraction in the tail is also much higher in this study ( f SFR = 22%) than in the GASP studies ( f SFR = 3%). Lee et al (2022) presented a detailed comparison of the star formation activity of the five jellyfish galaxies in this study with that of other known jellyfish galaxies including the GASP sample, considering galaxy stellar mass, redshift, and jellyfish morphology. As a result, they suggested a positive correlation between the star formation activity of jellyfish galaxies and the host cluster properties.…”

Section: Sfrs Gas Kinematics and Dynamical Statesmentioning

confidence: 99%

“…We display the projected phase-space diagrams of our targets and the GASP jellyfish galaxies (Gullieuszik et al 2020) by categorizing the sample based on stellar mass (Figure 12) and host cluster velocity dispersion (Figure 13). Lee et al (2022) showed the phase-space diagrams of the jellyfish galaxies with different categories of jellyfish morphology. We plot the 2D clustercentric distance normalized by the virial radius of the host cluster (R cl /R 200 ) on the x-axis, and we plot the velocity relative to the cluster normalized by the cluster velocity dispersion (|Δv los |/σ v,cl ) on the y-axis.…”

Section: Phase-space Of the Jellyfish Galaxiesmentioning

confidence: 99%

“…We carry out emission-line analyses of the GMOS/IFU data of jellyfish galaxies, which includes the Hα line. Using the Hα-derived SFRs of jellyfish galaxies in this study, Lee et al (2022) presented a relation between the star formation activity of the jellyfish galaxies and the host cluster properties. In this paper, we present detailed methods and analyses of emission lines of the jellyfish galaxies.…”

Section: Introductionmentioning

confidence: 99%

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A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters

Lee

Lee²,

Mun

et al. 2022

ApJ

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Jellyfish galaxies are an intriguing snapshot of galaxies undergoing ram pressure stripping (RPS) in dense environments, showing spectacular star-forming knots in their disks and tails. We study the ionized gas properties of five jellyfish galaxies in massive clusters with Gemini GMOS/Integral Field Unit observations: MACSJ0916-JFG1 (z = 0.330), MACSJ1752-JFG2 (z = 0.353), A2744-F0083 (z = 0.303), MACSJ1258-JFG1 (z = 0.342), and MACSJ1720-JFG1 (z = 0.383). “Baldwin, Phillips, and Terlevich” diagrams show that star formation, active galactic nuclei (AGNs), or mixed effects are ionizing gas in these galaxies. Radial velocity distributions of ionized gas seem to follow disk rotation of galaxies, with the appearance of a few high-velocity components in the tails as a sign of RPS. Mean gas velocity dispersion is lower than 50 km s−1 in most star-forming regions except near AGNs or shock-heated regions, indicating that the ionized gas is dynamically cold. Integrated star formation rates (SFRs) of these galaxies range from 7 M ⊙ yr−1 to 35 M ⊙ yr−1, and the tail SFRs are from 0.6 M ⊙ yr−1 to 16 M ⊙ yr−1, which are much higher than those of other jellyfish galaxies in the local universe. These high SFR values imply that RPS triggers intense star formation activity in these extreme jellyfish galaxies. The phase-space diagrams demonstrate that the jellyfish galaxies with higher stellar masses and higher host cluster velocity dispersion are likely to have more enhanced star formation activity. The jellyfish galaxies in this study have similar gas kinematics and dynamical states to those in the local universe, but they show a much higher SFR.

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Section: Phase-space Of the Jellyfish Galaxiessupporting

confidence: 59%

Section: Phase-space Of the Jellyfish Galaxiesmentioning

confidence: 98%

Section: Sfrs Gas Kinematics and Dynamical Statesmentioning

confidence: 99%

Section: Phase-space Of the Jellyfish Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters

Lee

Lee²,

Mun

et al. 2022

ApJ

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Dashing through the cluster: An X-ray to radio view of UGC 10420 undergoing ram-pressure stripping

Mahajan

Singh²,

Tiwari³

et al. 2023

Publ. Astron. Soc. Aust.

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We present multi-wavelength data and analysis, including new FUV AstroSat/UVIT observations of the spiral galaxy UGC 10420 (z = 0.032), a member of the cluster Abell 2199. UGC 10420 is present on the edge of the X-ray emitting region of the cluster at a distance of ∼ 680 kpc from the centre. The far-ultraviolet (FUV) data obtained by the AstroSat mission show intense knots of star formation on the leading edge of the galaxy, accompanied by a tail of the same on the diametrically opposite side. Our analysis shows that the images of the galaxy disk in the optical and mid-infrared are much smaller in size than that in the FUV. While the broadband optical colours of UGC 10420 are typical of a post-starburst galaxy, the star formation rate (SFR) derived from a UV-to-IR spectral energy distribution is at least a factor of nine higher than that expected for a star-forming field galaxy of similar mass at its redshift. A careful removal of the contribution of the diffuse intracluster gas shows that the significant diffuse X-ray emission associated with the inter-stellar medium of UGC 10420 has a temperature, and luminosity, L X = 1.8 ± 0.9 × 1040 erg s−1, which are typical of the X-ray emission from late-type spiral galaxies. Two symmetrically placed X-ray hot spots are observed on either sides of an X-ray weak nucleus. Our analysis favours a scenario where the interaction of a galaxy with the hot intra-cluster medium of the cluster, perturbs the gas in the galaxy causing starburst in the leading edge of the disk. On the other hand, the turbulence thus developed may also push some of the gas out of the disk. Interactions between the gas ejected from the galaxy and the intracluster medium can then locally trigger star formation in the wake of the galaxy experiencing ram-pressure stripping. Our data however does not rule out the possibility of a flyby encounter with a neighbouring galaxy, although no relevant candidates are observed in the vicinity of UGC 10420.

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Revealing the Relation between Star Formation Activity of Jellyfish Galaxies and Ram Pressure Stripping

Lee

Mun

et al. 2021

Proc. IAU

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Jellyfish galaxies are starburst galaxies with ram-pressure-stripped tails and blue star-forming knots. These galaxies show a snapshot of star formation enhancement triggered by ram pressure stripping (RPS), being important targets for studying the RPS-induced star formation in gas-rich galaxies. Here we investigate the star formation activity of five jellyfish galaxies in massive clusters, using Gemini GMOS/IFU observations. From the Hα-derived star formation rates (SFRs), we find that our sample shows higher SFR excess to the star formation main sequence than the jellyfish galaxies in low-mass clusters. From the compiled sample of jellyfish galaxies in low-mass to high-mass host clusters, we suggest that the star formation activity of jellyfish galaxies has positive correlations with host cluster mass and degree of RPS. These relationships imply that higher ram pressure environments tend to trigger stronger starbursts in jellyfish galaxies in the early stage of RPS.

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Enhanced Star Formation Activity of Extreme Jellyfish Galaxies in Massive Clusters and the Role of Ram Pressure Stripping

Cited by 13 publications

References 46 publications

A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters

A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters

Dashing through the cluster: An X-ray to radio view of UGC 10420 undergoing ram-pressure stripping

Revealing the Relation between Star Formation Activity of Jellyfish Galaxies and Ram Pressure Stripping

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