Pre-processing: an HI perspec ve
Eva Busekool PHISCC 2015 University of Groningen Kapteyn Astronomical ins tute
15-03-15 Eva Busekool - phiscc 2015 1 For the next 15 minutes…
• Introduc on • Ursa Major region • HI mass func on • Resolved HI imaging • Conclusions
15-03-15 Eva Busekool - phiscc 2015 2 Introduc on: Clusters
• Galaxy proper es are changing with environment
• Clusters studied in detail: rps
• Processes in groups?
R/R HI deficiency Frac on of S DEF > 0.30 A VIVA survey Solanis et al. (2001) 15-03-15 Eva Busekool - phiscc 2015 3 Introduc on: Groups Detec on frac on for each redshi shell • HI is a excellent tracer • Frac on of HI detec on decreases with increasing group size • What is really going on here?
Frac on of galaxies detected in HI Op cal group membership Hess et al. (2013)
Star-Forming frac on Log(Σ) [gal h2 Mpc-2] à Resolved HI imaging Cybulksi et al. 2014
15-03-15 Eva Busekool - phiscc 2015 4 HI imaging surveys of Ursa Major
• Ursa Major region – 17.4 Mpc – Dominated by late-types – No X-ray radia on • Targeted survey WSRT
– complete sample MB < -16.8 – 62 galaxies • Blind survey VLA-D – 54 poin ngs – 16% of volume – Θ = 45’’, Δv = 10.3 km/s, σ ~ 0.4 mJy/beam) – Main goal: construct HIMF Verheijen et al. (2001) 15-03-15 Eva Busekool - phiscc 2015 5 HIMF of the Ursa Major region
• HIMF of the Ursa Major region: – The slope is consistent with a flat slope – Slope is quite different than HIPASS and ALFALFA • Environmental dependence
15-03-15 Eva Busekool - phiscc 2015 6 HI morphologies
NGC 3985 NGC 3726
Credits: Davide Punzo 15-03-15 Eva Busekool - phiscc 2015 7 Interac ons NGC 4117/4118
NGC 3893/3896
15-03-15 Eva Busekool - phiscc 2015 8 Three brightest len culars NGC 4026 9 MHI = 1.2 x 10
NGC 3998/3990 8 MHI = 5.8 x 10 NGC 4111 9 MHI = 1.3 x 10
15-03-15 Eva Busekool - phiscc 2015 9 NGC 4111
15-03-15 Eva Busekool - phiscc 2015 10 HI morphologies
• Morphologies in HI – 40/58 have disturbed morphologies • Warps: 14 • HI distribu on lopsidedness: 11 • Kinema c lopsidedness: 15 • Interac ng: 15
à Very dynamical!
15-03-15 Eva Busekool - phiscc 2015 11 HI morphologies
warps warps 0.6 0.6 0.2 0.2 Morph Morph 0.6 0.6 lopsidedness lopsidedness 0.2 0.2
0.6 Kinema c 0.6 Kinema c lopsidedness lopsidedness 0.2 0.2
0.6 interac ons 0.6 interac ons 0.2 0.2 total 30 total 5 15 0 0 2 024680.2 0.00.20.40.60.81.01.2 − − types log Σ (gal/Mpc2)
15-03-15 Eva Busekool - phiscc 2015 12 HI proper es 3
K 2
/L 1 HI 0
log M 1 − 2 − 2.5 25 /D
HI 1.5 D
0.5 0.006
2 HI 0.004 /D HI
M 0.002
0.000 1 135790.2 0.00.20.40.60.81.0 − − type log Σ (gal/Mpc2)
15-03-15 Eva Busekool - phiscc 2015 13 Take home message
• The slope of the HIMF of the UMa region is consistent with a flat slope. This could be a hint towards environmental dependence and/or pre- processing • The Ursa Major region is very dynamical Lot of warps, lopsidedness and interac ons. • Three brightest len culars have huge HI tails This could be stripping and transforma on from a spiral to a len cular
15-03-15 Eva Busekool - phiscc 2015 14 Morphology-density rela on
10
8
6
4
2 morph type
0
2 −
4 − 0.2 0.00.20.40.60.81.01.2 − log Σ (gal/Mpc2)
15-03-15 Eva Busekool - phiscc 2015 15 Interac ons NGC 4117/4118
NGC 3893/3896
15-03-15 Eva Busekool - phiscc 2015 16 VLA imaging mosaic of Ursa Major
• 41 galaxies detected 7 (M HI, min ~ 10 Msun) • Science goals: – Study HI morphology and kinema cs – Slope of HIMF
15-03-15 Eva Busekool - phiscc 2015 Eva Busekool 17 Pre-processing?
• NGC 4026 and NGC 3938 group inside UMa region – FOF (Wolfinger, PhD thesis) • HI frac on ~ 70%
15-03-15 Eva Busekool - phiscc 2015 18 NGC 4088/4085
15-03-15 Eva Busekool - phiscc 2015 19