The Type Ia Supernova 1998bu in M96 and the Hubble Constant

Jha, Saurabh W.; Garnavich, P.; Kirshner, R.; Challis, Peter; Söderberg, A. M.; Macri, Lucas M.; Huchra, J. P.; Barmby, P.; Barton, Elizabeth J.; Berlind, P.; Brown, Warren R.; Caldwell, Nelson; Calkins, M.; Kannappan, Sheila J.; Koranyi, D.; Pahre, M. A.; Rines, Kenneth J.; Stanek, K. Z.; Stefanik, R. P.; Szentgyörgyi, Á.; Vaïsänen, P.; Wang, Z.; Zajac, Joseph; Riess, Adam G.; Filippenko, A. V.; Li, W.; Modjaz, M.; Treffers, R. R.; Hergenrother, C. W.; Grebel, Eva K.; Seitzer, Patrick; Jacoby, George H.; Benson, P. J.; Rizvi, Akbar; Marschall, Laurence A.; Goldader, J. D.; Beasley, Michael A.; Vacca, William D.; Leibundgut, B.; Spyromilio, J.; Schmidt, B.; Wood, P. R.

doi:10.1086/313275

Cited by 177 publications

(97 citation statements)

References 140 publications

(208 reference statements)

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“…Recently, Tammann & Reindl (2013) derived M V ,max = −19.45 ± 0.15 for SN 1989B and M V ,max = −19.38 ± 0.16 for SN 1998bu from the photometry in the literature Jha et al 1999;Hernandez et al 2000;Wells et al 1994), adopting a mean TRGB distance of the Leo I Group, (m − M) 0 = 30.39 ± 0.10. These values were obtained after correcting for the Galactic extinction, host galaxy extinction, and decline rates (Δm 15 ).…”

Section: The Calibration Of the Absolute Magnitudes Of Sne Ia And Thementioning

confidence: 99%

“…M66 (NGC 3627, SAB(s)b) and M96 (NGC 3368, SAB(rs)ab) are nearby bright spiral galaxies hosting SNe Ia: SN 1989B in M66 (Evans & McNaught 1989;Wells et al 1994) and SN 1998bu in M96 (Villi et al 1998;Suntzeff et al 1999;Jha et al 1999;Hernandez et al 2000;Spyromilio et al 2004). M66 has been host to other three SNe as well: SN II 1973R (Ciatti & Rosino 1977), SN imposter SN 1997bs (Van Dyk et al 2000, and SN II-L 2009hd (Elias-Rosa et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

Lee

Jang

2013

ApJ

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M66 and M96 in the Leo I Group are nearby spiral galaxies hosting Type Ia supernovae (SNe Ia). We estimate the distances to these galaxies from the luminosity of the tip of the red giant branch (TRGB). We obtain VI photometry of resolved stars in these galaxies from F555W and F814W images in the Hubble Space Telescope archive. From the luminosity function of these red giants, we find the TRGB I-band magnitude to be I TRGB = 26.20 ± 0.03 for M66 and 26.21 ± 0.03 for M96. These values yield distance modulus (m − M) 0 = 30.12 ± 0.03(random) ± 0.12(systematic) for M66 and (m − M) 0 = 30.15 ± 0.03(random) ± 0.12(systematic) for M96. These results show that they are indeed the members of the same group. With these results we derive absolute maximum magnitudes of two SNe (SN 1989B in M66 and SN 1998bu in M96). V-band magnitudes of these SNe Ia are ∼0.2 mag fainter than SN 2011fe in M101, one of the nearest recent SNe Ia. We also derive near-infrared magnitudes for SN 1998bu. Optical magnitudes of three SNe Ia (SN 1989B, SN 1998bu, and SN 2011fe)

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Section: The Calibration Of the Absolute Magnitudes Of Sne Ia And Thementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

Lee

Jang

2013

ApJ

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“…A comparable number of relatively normal SNe Ia have also been individually studied, including SNe 1994D (Patat et al 1996), 1996X (Salvo et al 2001), 1998aq (Branch et al 2003;Riess et al 2005), 1998bu (Jha et al 1999), 1999ee (Stritzinger et al 2002;Hamuy et al 2002), 2001el (Krisciunas et al 2003), 2002er (Pignata et al 2004;Kotak et al 2005), 2003cg (Elias-Rosa et al 2006, 2003du (Stanishev et al 2007), 2004eo (Pastorello et al 2007a), 2002bo (Benetti et al 2004), and 2006X (Wang et al 2008a), though the last two may differ from other typical SNe Ia given the unusually high expansion velocity of their photospheres and a relatively flat evolution of their B-band light curves starting from the early nebular phase (Wang et al 2008a). However, a much larger sample of SNe Ia must be investigated in order to determine the dispersion among their properties and refine possible systematic effects for precision cosmology.…”

Section: Introductionmentioning

confidence: 99%

THE GOLDEN STANDARD TYPE Ia SUPERNOVA 2005cf: OBSERVATIONS FROM THE ULTRAVIOLET TO THE NEAR-INFRARED WAVEBANDS

Wang

Filippenko

et al. 2009

ApJ

159

160

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We present extensive photometry at ultraviolet (UV), optical, and near-infrared (NIR) wavelengths, as well as dense sampling of optical spectra, for the normal Type Ia supernova (SN Ia) 2005cf. The optical photometry, performed at eight different telescopes, shows a 1σ scatter of 0.03 mag after proper corrections for the instrument responses. From the well-sampled light curves, we find that SN 2005cf reached a B-band maximum at 13.63 ± 0.02 mag, with an observed luminosity decline rate Δm 15 (B) = 1.05 ± 0.03 mag. The correlations between the decline rate and various color indexes, recalibrated on the basis of an expanded SN Ia sample, yield a consistent estimate for the host-galaxy reddening of SN 2005cf, E(B − V ) host = 0.10 ± 0.03 mag. The UV photometry was obtained with the Hubble Space Telescope and the Swift Ultraviolet/Optical Telescope, and the results match each other to within 0.1-0.2 mag. The UV light curves show similar evolution to the broadband U, with an exception in the 2000-2500 Å spectral range (corresponding to the F220W/uvm2 filters), where the light curve appears broader and much fainter than that on either side (likely owing to the intrinsic spectral evolution). Combining the UV data with the ground-based optical and NIR data, we establish the generic UVoptical-NIR bolometric light curve for SN 2005cf and derive the bolometric corrections in the absence of UV and/or NIR data. The overall spectral evolution of SN 2005cf is similar to that of a normal SN Ia, but with variety in the strength and profile of the main feature lines. The spectra at early times displayed strong, high-velocity (HV) features in the Ca ii H&K doublet and NIR triplet, which were distinctly detached from the photosphere (v ≈ 10,000 km s −1 ) at a velocity ranging from 20,000 to 25,000 km s −1 . One interesting feature is the flatbottomed absorption observed near 6000 Å in the earliest spectrum, which rapidly evolved into a triangular shape and then became a normal Si ii λ6355 absorption profile at about one week before maximum brightness. This premaximum spectral evolution is perhaps due to the blending of the Si iiλ6355 at photospheric velocity and another HV absorption component (e.g., an Si ii shell at a velocity ∼18,000 km s −1 ) in the outer ejecta, and may be common in other normal SNe Ia. The possible origin of the HV absorption features is briefly discussed.

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“…For over a decade, Type Ia supernovae (SNe Ia) have widely been used as a cosmological distance indicator to directly probe the accelerating expansion of the universe (Riess et al 1996;Perlmutter et al 1997Perlmutter et al , 1999Astier et al 2006) and measure the Hubble constant H 0 (Jha et al 1999). In addition, supernovae (SNe) are critical in the study of star formation history and the chemical evolution of the universe (Sharon et al 2007).…”

Section: Introductionmentioning

confidence: 99%

THE PROPERTIES OF TYPE Ia SUPERNOVA HOST GALAXIES FROM THE SLOAN DIGITAL SKY SURVEY

Han

Park

Choi

et al. 2010

ApJ

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We investigate the properties and environments of Type Ia Supernova (SN Ia) host galaxies in the Stripe 82 of the Sloan Digital Sky Survey-II Supernova Survey centered on the celestial equator. Host galaxies are defined as the galaxy nearest to the supernova (SN) in terms of angular distance whose velocity difference from the SN is less than 1000 km s −1 . Eighty seven SN Ia host galaxies are selected from the SDSS Main galaxy sample with the apparent r-band magnitude m r < 17.77, and compared with the SDSS Main galaxies. The SN Ia rates for early-and late-type galaxies are 0.81 ± 0.19 SN (100 yr) −1 and 0.99 ± 0.21 SN (100 yr) −1 , respectively. We find that the host galaxies have a color distribution consistent with that of the Main galaxies, regardless of their morphology. However, host galaxies are on average brighter than the Main galaxies by ∼0.3 mag over the range of −18.3 > M r > −21.3. But the brighter ends of their luminosity distributions are similar. The distribution of the distance to the nearest neighbor galaxy shows that SNe Ia are more likely to occur in isolated galaxies without close neighbors. We also find that the SN Ia host galaxies are preferentially located in a region close to massive galaxy clusters compared to the Main galaxies.

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The Type Ia Supernova 1998bu in M96 and the Hubble Constant

Cited by 177 publications

References 140 publications

THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

THE GOLDEN STANDARD TYPE Ia SUPERNOVA 2005cf: OBSERVATIONS FROM THE ULTRAVIOLET TO THE NEAR-INFRARED WAVEBANDS

THE PROPERTIES OF TYPE Ia SUPERNOVA HOST GALAXIES FROM THE SLOAN DIGITAL SKY SURVEY

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