A New Perspective on Galaxy Outflows Glenn Kacprzak Kutching - Sept. 19 th 2014 N. Bouché (IRAP) C. Churchill (NMSU) J. Cooke (Swinburne) S. Ho (UCSB) E. Klimek (NMSU) A. LeReun (IRAP) C. Martin (UCSB) N. Nielsen (NMSU) I. Schroetter (IRAP)

How We Observe Outflows Transverse Absorption MgII

Kacprzak et al Transverse Absorption

Kacprzak et al 2012 Also see: Bordoloi et al. 2011, Bouche et al. 2012, Lan et al Kacprzak et al. 2013

Transverse Absorption Lehner et al. 2013Kacprzak et al 2012 Also see: Bordoloi et al. 2011, Bouche et al. 2012, Lan et al

Two-Point Correlation Function The TPCF is obtained by taking the velocity differences between all pixel pairs in each system and binning them in velocity.

How We Observe Outflows Down-the-Barrel Absorption MgII

Weiner et al Also see: Martin & Bouche 2009, Rubin et al. 2010, Steidel et al. 2010, Martin et al. 2012, Rubin et al. 2012, Bordoloi et al Down-the-Barrel Absorption Bordoloi et al 2013

How We Observe Outflows Wouldn’t it be great to do both at the same time? No examples of this yet until now Kacprzak et al 2014, ApJL, 792, 12

Keck/LRIS slit placed on the quasar and galaxy APO/DIS slit placed along the major-axis of the galaxy D=58 kpc i = 52 ± 5 degrees Quasar 3 degrees from minor axis Probing Transverse + Down-the-Barrel Absorption Kacprzak et al 2014

Blueshifted “Down-the-Barrel” and “Transverse” MgII wrt Ha [O/H] = -0.21±0.08 SFR = Msun/yr Kacprzak et al 2014 Probing Transverse + Down-the-Barrel Absorption

Martin et al model Single v=-45 ± 15 km/s Modeling Down-the-Barrel Absorption Fixed ISM - width=200 km/s Double v=-132 ± 25 km/s Correct for inclination -v dtb = km/s Kacprzak et al 2014

Bouché et al outflow model - constant winds - populated with 10 5 clouds - half opening angle = degrees - perpendicular to the disk Modeling Transverse Absorption Kacprzak et al 2014

Best fit models yield v out =40-80 km/s This overlaps with v dtb = km/s Bouché et al outflow model - constant winds - populated with 10 5 clouds - half opening angle = degrees - perpendicular to the disk Kacprzak et al 2014 Modeling Transverse Absorption

Absorption Metallicity Kacprzak et al 2014

Absorption Metallicity log N(HI) = ± 0.15 Transverse: < X/H < -1.1 Kacprzak et al 2014 Galaxy : [O/H] = -0.21±0.08 If it is outflow, then we derive an gas outflow rate Msun/yr And for galaxy SFR= Msun/yr -> Mass loading factor =

Summary First detection of blueshifted down-the-barrel and transverse absorption. Both down-the-barrel and transverse models reproduce the absorption velocities indicating a kinematic connection. The combined geometry, kinematics and metallicity are suggestive that it is an outflow. The metallicity gradient from the galaxy (-0.21) to 58 kpc (-1.1) is suggestive that the gas is diluted or mixed during its journey.