HI Observations of Galaxies in the Filaments/Groups around Virgo Hyein Yoon (윤혜인; Yonsei University) MCG-01-33-059 (GMRT) NGC 5116 (JVLA) UGC 07143 (WSRT) HI (contour) + Optical Aeree Chung (Yonsei), Chandreyee Sengupta (Yonsei), Jacqueline van Gorkom (Columbia), Martin Bureau (Oxford), O. Ivy Wong (ICRAR/UWA), Shan Huang (NYU), Soo-Chang Rey (CNU) 2018 Radio Telescope User’s Meeting (KASI) Environmental Processes in Galaxy Clusters Interactions between galaxies and their surroundings in clusters Gravitational Interactions ICM-ISM Interactions § Galaxy-Galaxy interaction § Ram pressure stripping (Mihos 2004) (Gunn & Gott 1972) § Galaxy harassment § Thermal evaporation (Moore et al. 1996) (Cowie & Songaila 1977) § Galaxy-Cluster interaction § Turbulent-viscous stripping (Byrd & Valtonen 1990, Bekki 1999) (Nulsen 1982) Galaxy-Galaxy interaction NGC 4567 Ram-pressure stripping NGC 4522 (Credit : C. Mihos, and C. McBride) NGC 4568 (Credit : B. Vollmer) (Chung+ 2009) (Chung+ 2009) 2 Environmental Processes in Galaxy Clusters Interactions between galaxies and their surroundings in clusters (e.g. ICM-ISM interactions within R200 of Virgo) VIVA II project 48 spiral galaxies located throughout the Virgo cluster (VIVA I: Chung+2009) High resolution HI data (VLA) + Impact of local environments ➔ 35 galaxies have signs of “Gas stripping” ICM-ISM interactions: - Early stage (Yoon+ 2017) - Active stage - Past stage - Slow process 3 Environmental Processes in Galaxy Clusters Interactions between galaxies and their surroundings in clusters (e.g. ICM-ISM interactions within R200 of Virgo) Early stage of N4396 VIVA II project gas stripping stellar disk Optical + HI (contour) Most active gas stripping N4522 ICM-ISM interactions: Gas stripped - Early stage - Active stage in the past - Past stage - Slow process N4405 4 Chung+ 2009 Environmental Processes in the Outskirts of Clusters Galaxies may already get affected by their surroundings before they arrive in the core of the cluster (“Pre-processing”) VIVA II project ICM-ISM interactions: - Early stage - Active stage - Past stage - Slow process 5 Environmental Processes in the Outskirts of Clusters Galaxies may already get affected by their surroundings before they arrive in the core of the cluster (“Pre-processing”) VIVA II project Gas stripping? N4698 stellar disk Optical + HI (contour) Gas accretion? N4808 ICM-ISM interactions: - Early stage - Active stage Chung+ 2009 - Past stage - Slow process 6 N4405 “Pre-processing” of Galaxies in the Outskirts of Clusters Galaxies may already get affected by their surroundings before they arrive in the core of the cluster (“Pre-processing”) Solanes+ 2001 ← A good fraction of HI-deficient galaxies in cluster outskirts poor galaxies - Fraction of Recent studies on pre-processing: gas 1.5 • Low HI detections (processed HI) 1.0 in group environments (Mhalo 0.5 dependence) - Hess and Wilcots 2013 0.0 • Gas-poor and red galaxies HI deficiency HI in infalling regions of Abell 963 - 0.5 0 1 2 3 4 5 - BUDHIES II: Jaffé+ 2015 r / RABELL • Lower star formation rate in groups/filaments around Coma supercluster - Cybulski+ 2014 7 HI Imaging Study of Galaxies in Virgo Filaments/Groups Key Questions: § Can we detect any observational evidence on gas morphologies that galaxies be “pre-processed” in low-density environments? § What kinds of physical processes can take place in infalling structures? (e.g. Gas accretion or Gas stripping + Tidal interactions) § How does the pre-processing during the infalling would enhance the galaxy evolution within the cluster? To answer the above questions: High resolution HI imaging study of 14 late-type galaxies in the filaments/groups around the Virgo cluster 8 HI Detections (Single dish) in Virgo Filaments/Groups ] 1 - [ km s [ km cz DEC. (2000) DEC. Virgo Color: radial velocity (cz) Size: HI gas mass (single dish) - ALFALFA (Arecibo) - HIPASS (Parkes) - LEDA (inhomogeneous) 9 R.A. (2000) HI Observations of Galaxies in Virgo Filaments/Groups NE Filament NW Filament (sheet-like) JVLA WSRT (D) (72m) NGC 5116 cz[km/s] NGC 5116 cz[km/s] NGC 5116 DEC. (2000) DEC.(2000) Virgo DEC. (2000) Virgo Virgo GMRTCluster Virgo Virgo 3 gas-poor Cluster Cluster Virgo DEC. (2000) DEC. Cluster Cluster 2 gas-rich ~ 124 hours ~ 3-5 x 1019 cm-2 7 gas-rich SE Infalling Virgo Int. R.A. (2000) Virgo Telescope Obs. time BW # of Group (array) date Virgo (MHz) Chan. Cluster (hr) Cluster Cluster VLA July Aug 1.5 x 5 NE (D-array) 16.00 512 (CASA) 2014 ~ 8 hrs (~ 3400 km/s) (1 chan ~ 7 km/s) 12 x 5 WSRT Dec 2013 / 20.00 1024 DEC. (2000) NW (72m) Jan Apr May + 18 x 2 DEC. (2000) (~ 4300 km/s) (1 chan ~ 4 km/s) (MIRIAD)DEC. (2000) July Aug 2014 1 gas-poor ~ 96 hrs 10 x 2 512 1 gas-poor SE GMRT Jan 2014 16.67 (AIPS) ~ 20 hrs (~ 3400km/s) (1 chan ~ 7 km/s)10 R.A.R.A. (2000) (2000) R.A. (2000) R.A. (2000) HI Imaging: Gas-richer Galaxies ➔ Gas Accretion? MCG-01-33-059 (GMRT) • Very extended and SE infalling group asymmetric gas disk • High gas content • Distorted velocity field and warp • No obvious neighbors D ~ 1.5’ • Star forming regions Optical P-V diagram HI (blue, GMRT) Optical (red, DSS) Optical Hα (green, OHP) along (Lowest HI contour level: 3.4 x 1019 cm -2) minor mom 1 • DHI/Dopt ~ 3.80 • def HI ~ - 0.61 • log (MHI/LB) = - 0.01 GALEX 11 HI Imaging: Gas-richer Galaxies ➔ Gas Accretion? MCG-01-33-059 (GMRT) DHI/Dopt ~ 3.8 UGC 07039 (WSRT) DHI/Dopt ~ 3.1 SE Infalling Group def HI ~ -0.61 NW filament def HI ~ -0.84 Optical mom 1 + HI (contour) (Lowest HI contour level: 3.4 x 1019 cm -2) (Lowest HI contour level: 4.0 x 1019 cm -2) IC 0777 (WSRT) DHI/Dopt ~ 2.5 NGC 4152 (WSRT) DHI/Dopt ~ 2.0 NW filament def HI ~ -0.70 NW filament def HI ~ -0.66 (Lowest HI contour level: 5.4 x 1019 cm -2) (Lowest HI contour level: 5.0 x 1019 cm -2) 12 HI Content: Gas-richer Galaxies ➔ Gas Accretion? def HI vs Clustocentric distance 1.5 1.0 log (MHI/M*) vs log M* 0.5 U7186 HI deficiency HI 0.0 P1760270 ) -0.5 * U7039 0 1 2 3 4 5 /M r / RABELL HI P38859 U7143 Solanes+ 2001 M ( IC777 og > N4152 0 l B /L HI -1 <M -2 og l 12 E S0 S0a Sa Sab Sb Sbc Sc Scd Sd Sm Im log M* log (MHI/LB) vs Morphology Huang+ 2012 Roberts & Haynes 1994 13 HI Imaging: Gas-poorer Galaxies ➔ Gas Stripping? IC 3908 (GMRT) SE infalling group • One-sided weak gas tail HI mom 0 (blue, GMRT) • Asymmetric but not Optical (red, DSS) truncated (yet) Hα (green, OHP) • Low/normal gas content • Red optical disk D ~ 1.8’ P-V diagram Optical along major mom 1 (Lowest HI contour level: 3.5 x 1019 cm -2) • DHI/Dopt = ~ 1.50 • def HI ~ 0.04 14 • log (MHI/LB) ~ - 0.74 HI Imaging: Gas-poorer Galaxies ➔ Gas Stripping? IC 3908 (GMRT) DHI/Dopt ~ 1.50 SE infalling group def HI ~ 0.04 (Lowest HI contour level: 3.5 x 1019 cm -2) NGC 5116 (JVLA) DHI/Dopt ~ 1.80 NE filament def HI ~ 0.15 (Lowest HI contour level: 6.1 x 1019 cm -2) 15 HI Imaging: Gas-poorer Galaxies ➔ Gas Stripping? D /D ~ 1.50 IC 3908 (GMRT) HI opt Similar to Virgo galaxies SE infalling group def HI ~ 0.04 in the early stage of gas stripping one (no truncation, - sided extension) (Lowest HI contour level: 3.5 x 1019 cm -2) NGC 5116 (JVLA) DHI/Dopt ~ 1.80 NE filament def HI ~ 0.15 (Lowest HI contour level: 6.1 x 1019 cm -2) DHI/DB 16 HI Content: Gas-poorer Galaxies ➔ Gas Stripping? def HI vs Clustocentric distance 1.5 1.0 NGC 5240 log (MHI/M*) vs log M* 0.5 UGC 08662 HI deficiency HI 0.0 ) -0.5 * 0 1 2 3 4 5 /M HI U8662 Solanes+ 2001 r / RABELL M ( N5116 og > 0 l B N5240 /L HI -1 <M -2 og l 12 E S0 S0a Sa Sab Sb Sbc Sc Scd Sd Sm Im log M* Huang+ 2012 log (MHI/LB) vs Morphology Roberts & Haynes 1994 17 HI Imaging: Potentially Interacting Pairs UGC 07143 (WSRT) Optical – right; NW filament • DHI/Dopt ~ 3.84 • def HI = - 0.55 d ~ 13 kpc • Close neighbor (left): Δv ~ 17 km/s SDSS J120958.86+250106.3 (Lowest contour level: 6.3 x 1019 cm -2) PGC 038859 (WSRT) - left; NW filament • DHI/Dopt ~ 7.90 • def HI ~ - 0.63 • Close neighbor (right): NGC 4158 (Lowest contour level: d ~ 70 kpc 3.1 x 1019 cm -2) Δv ~ 20 km/s 18 Extended Study: Star Formation and HI Gas in Virgo Field 1. Mapping the star formation and HI gas properties in three Virgo filaments and two groups è NUV-r, W3-W1, g-r colors and HI content color: NUV - r size: stellar mass Voronoi 2. Statistical analysis with all galaxies in Virgo field (1800 < cz < 3300 km/s) NUV-r vs log M* log(MHI/M*) vs log M* MST Cluster Group Filament Void 19 Yoon+ in prep Summary • We carried out 124 hours HI observations by using the GMRT, JVLA and WSRT to find observational signatures of environmental processes in Virgo filaments/groups. • Our galaxies show intriguing morphological peculiarities in HI, suggesting “pre-processing” in the low-density environments. è - Gas accretion: extended gas-rich disk, asymmetry in velocity field - Gas stripping: one-sided tail (early stage), no truncations - Interacting pairs • In addition, we mapped the stellar and gas properties of galaxies in large-scale environments around Virgo field.