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Spatially-Resolved Dust and Gas Properties of the GRB 980425 Host Galaxy

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Spatially-Resolved Dust and Gas Properties of the GRB 980425 Host Galaxy Introduction New data Science highlights Spatially-resolved dust and gas properties of the GRB 980425 host galaxy Michał Jerzy Michałowski /me-how me-how-ov-ski/ Institute for Astronomy, University of Edinburgh 16.04.2015 ALMA/Herschel Archival Workshop, ESO 1/13 Introduction New data Science highlights Outline 1 Introduction 2 New data 3 Science highlights 2/13 Introduction New data Science highlights SFH from the gamma-ray burst (GRB) rate t [Gyr] 13 8 4 2 1 0.6 1 ] -3 0.1 Mpc -1 -2 10 GRB: (evolution corrected) [M yr LBG: Bouwens et al. (2008) * -3 . ρ 10 B08 (LF integrated) LAE: Ota et al. (2008) ρ c (C / fesc = 40, 30, 20) -4 10 0 1 2 3 4 5 6 7 8 9 z Kistler et al. (2009, ApJ, 705, 104) 3/13 Introduction New data Science highlights Are GRBs good tracers of cosmic star formation? Biased tracers Perley et al. (2013, ApJ, Unbiased tracers 778, 128; 2015, ApJ, 801, Michałowski et al. (2012, 102): mass ApJ, 755, 85): radio Boissier et al. (2013, A&A, Perley et al. (2013, ApJ, 557, 34): mass 778, 172; 2015, ApJ, 801, Vergani et al. (2015, A&A, 102): radio submitted, Hunt et al. (2014, A&A, arXiv:1409.7064): 565, 112): Herschel mass Kohn et al. (2015, MNRAS, Schulze et al. (2015, A&A, 448, 1494): Herschel submitted, arXiv:1503.04246): metallicity 4/13 Introduction New data Science highlights GRB 980425 z = 0.0085 (the closest GRB) the first confirmed SN association half-light diameter = 22′′ (4 kpc) WR region dominating the 24 µm flux 5/13 Introduction New data Science highlights Previous multi-wavelength data X-ray FUV NUV U WR region SN site 10’’ 1.75 kpc B V R I J H K 4.5 µ m 8.0 µ m 24 µ m Michałowski et al. (2009, ApJ, 693, 347) 6/13 Introduction New data Science highlights Spitzer 70–160 µm imaging Le Floc’h et al. (2012, ApJ, 746, 7) 7/13 0.20 µm 0.22 µm 0.26 µm R-band 100 µm 160 µm 250 µm 350 µm 500 µm 870 µm 2.8 mm 1.75 kpc 10 arcsec 10 cm 13 cm 16 cm 23 cm Introduction New data Science highlights Spectral energy distribution Entire host WR region Host-WR 10-1 LMC MAGPHYS models GRASIL models Spitzer/IRS spectrum 10-2 Flux density (Jy) 10-3 10-4 10-1 100 101 102 103 104 105 Observed wavelength (µm) 9/13 Introduction New data Science highlights Low dust content: recent re-start of star-formation -2.0 -2.5 ) * / M -3.0 d -3.5 log(M GRB 980425 host LMC HI-normal HI-deficient -4.0 Outside Virgo Virgo KINGFISH -4.5 2 3 4 5 NUV - r (mag) 10/13 Introduction New data Science highlights WR region: dense ISM WR region GRB/SN site ) 300 -3 Other regions (cm e 200 100 Electron density, n 0 2 4 6 8 10 Age (Myr) 11/13 Introduction New data Science highlights WR region: dense ISM WR region GRB/SN site ) 300 -3 Other regions (cm e 200 100 Electron density, n 0 2 4 6 8 10 Age (Myr) 11/13 Introduction New data Science highlights Submm excess 870 µm flux higher by a factor of two than the model prediction low 160 µm/ 870 µm ∼ 25 either double the Mdust or shallow β = 1 ALMA 2.8mm: the WR region is responsible? 12/13 Introduction New data Science highlights Submm excess 870 µm flux higher by a factor of two than the model prediction low 160 µm/ 870 µm ∼ 25 either double the Mdust or shallow β = 1 ALMA 2.8mm: the WR region is responsible? Galametz et al. (2011, A&A, 532, A56) 12/13 Introduction New data Science highlights Submm excess 870 µm flux higher by a factor of two than the model prediction low 160 µm/ 870 µm ∼ 25 either double the Mdust or shallow β = 1 ALMA 2.8mm: the WR region is responsible? Galametz et al. (2011, A&A, 532, A56) 12/13 Introduction New data Science highlights Submm excess 870 µm flux higher by a factor of two than the model prediction low 160 µm/ 870 µm ∼ 25 either double the Mdust or shallow β = 1 ALMA 2.8mm: the WR region is responsible? Galametz et al. (2011, A&A, 532, A56) 12/13 Introduction New data Science highlights Conclusions Low dust content: evidence for a recent re-start of star-formation Submm excess: very cold dust, or shallow β WR region: dominates at far-infrared and radio WR region: dense ISM Details in Michałowski et al (2014, A&A, 562, 70) 13/13.
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