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What can low- z LAEs tell us about high- z ones … and vice versa. Göran Östlin W ith a little help from my friends. 1.8 arcminutes (2.1 kpc) wide. F336W (U), F502N ([O III]), F555W (V), F656N (H-alpha), F702N (R), F814W (I) . ESO 338-04 (a.k.a. Tol1924-416 ) M B = -19
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What can low-zLAEs tell us about high-z ones … and vice versa GöranÖstlin With a little help from my friends
1.8 arcminutes (2.1 kpc) wide. F336W (U), F502N ([O III]), F555W (V), F656N (H-alpha), F702N (R), F814W (I)
ESO 338-04 (a.k.a. Tol1924-416) MB= -19 12+log(O/H) = 8.1 SFR = 4 Msun/yr Log(LFUV)) = 10 Log(LLyα)) = 41.9 EW(Hα) = 600 Å EW(Lyα) = 30 Å D(HI) = 10 kpc 20x20 arcsec, 3.5 x 3.5 kpc
Summary of Lyα results from low z • UV spectroscopy reveal the importance of ISM kinematics • Lyα seen from dusty regions • Lyα seen far from the production sites • Globally Lyα not a function of metallicity • Globally fesc,Lyα anti-”corelated” with E(B-V) • GloballyW(Lyα) anticorelated with W(Hα) • ISM kinematic evolution? • Large pop of high-zHAEs not seen in Lyα? • Resonant scattering, ISM kin, porosity – all contribute • Are the underlying high/low-z physics driving SF the same? • yes and no / quiescent vs violent • Caveat: small and biased sample at low-z