The first year of SN 2004dj in NGC 2403★

Vinkó, J.; Takáts, K.; Sárneczky, K.; Szabó, Gy. M.; Mészáros, Szabolcs; Csorvási, R.; Szalai, T.; Gáspár, András; Pál, András; Csizmadia, Sz.; Kóspál, Á.; Rácz, Miklós Z.; Kun, M.; Csák, B.; Fürész, Gábor; DeBond, Heide; Grunhut, J.; Thomson, James Robertson; Mochnacki, S. W.; Koktay, T.

doi:10.1111/j.1365-2966.2006.10416.x

Cited by 61 publications

(107 citation statements)

References 49 publications

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“…This is somewhat larger than the heliocentric velocity of the nuclear region of NGC 2403 of ∼130 km s −1 given in the SIMBAD and NED databases, but this is not surprising given the likely dispersion of velocities within the host galaxy. Indeed, Vinkó et al (2006) point out that H i mapping of NGC 2403 (Fraternali et al 2001) suggests that the true radial velocity of the SN 2004dj barycenter is about +221 km s −1 . We adopt this value here.…”

Section: Sn 2004djmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle¹,

Kotak²,

Farrah³

et al. 2011

ApJ

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We present mid-infrared (MIR) spectroscopy of a Type II-plateau supernova, SN 2004dj, obtained with the Spitzer Space Telescope, spanning 106-1393 days after explosion. MIR photometry plus optical/near-IR observations are also reported. An early-time MIR excess is attributed to emission from non-silicate dust formed within a cool dense shell (CDS). Most of the CDS dust condensed between 50 days and 165 days, reaching a mass of 0.3 × 10 −5 M . Throughout the observations, much of the longer wavelength (>10 μm) part of the continuum is explained as an IR echo from interstellar dust. The MIR excess strengthened at later times. We show that this was due to thermal emission from warm, non-silicate dust formed in the ejecta. Using optical/near-IR line profiles and the MIR continua, we show that the dust was distributed as a disk whose radius appeared to be shrinking slowly. The disk radius may correspond to a grain destruction zone caused by a reverse shock which also heated the dust. The dust-disk lay nearly face-on, had high opacities in the optical/near-IR regions, but remained optically thin in the MIR over much of the period studied. Assuming a uniform dust density, the ejecta dust mass by 996 days was (0.5 ± 0.1) × 10 −4 M and exceeded 10 −4 M by 1393 days. For a dust density rising toward the center the limit is higher. Nevertheless, this study suggests that the amount of freshly synthesized dust in the SN 2004dj ejecta is consistent with that found from previous studies and adds further weight to the claim that such events could not have been major contributors to the cosmic dust budget.

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Section: Sn 2004djmentioning

confidence: 99%

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

Meikle¹,

Kotak²,

Farrah³

et al. 2011

ApJ

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“…NGC 2403 is the only galaxy whose distance differs from Walter et al (2008). We used the estimate of the distance given in Vinkó et al (2006) because it comes from more numerous and more recent data. We remind the reader that a fit with a 0 free and the distance fixed is equivalent to a fit with the distance free and a 0 fixed (Begeman et al 1991), because the observed total gravitational acceleration is proportional to 1/D, where D is the distance.…”

Section: The Acceleration Constant Amentioning

confidence: 99%

THINGS about MOND

Gentile

Famaey

Blok

2011

A&A

154

219

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We present an analysis of 12 high-resolution galactic rotation curves from The HI Nearby Galaxy Survey (THINGS) in the context of modified Newtonian dynamics (MOND). These rotation curves were selected to be the most reliable for mass modelling, and they are the highest quality rotation curves currently available for a sample of galaxies spanning a wide range of luminosities. We fit the rotation curves with the "simple" and "standard" interpolating functions of MOND, and we find that the "simple" function yields better results. We also redetermine the value of a 0 , and find a median value very close to the one determined in previous studies, a 0 = (1.22 ± 0.33) × 10 −8 cm s −2 . Leaving the distance as a free parameter within the uncertainty of its best independently determined value leads to excellent quality fits for 75% of the sample. Among the three exceptions, two are also known to give relatively poor fits in Newtonian dynamics plus dark matter. The remaining case (NGC 3198) presents some tension between the observations and the MOND fit, which might, however, be explained by the presence of non-circular motions, by a small distance, or by a value of a 0 at the lower end of our best-fit interval, 0.9 × 10 −8 cm s −2 . The best-fit stellar M/L ratios are generally in remarkable agreement with the predictions of stellar population synthesis models. We also show that the narrow range of gravitational accelerations found to be generated by dark matter in galaxies is consistent with the narrow range of additional gravity predicted by MOND.

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“…For 25 SNe we estimate this quantity by measuring the peak wavelength of the narrow emission lines resulting from the superposed H ii region (e.g., Leonard et al 2002b). For the other 22 SNe the aforementioned emission line is not detected, so we adopt the redshift of the host galaxy nucleus, while for SN 1991al, SN 1999em, and SN 2004dj we adopt the values from Hamuy (2001), Leonard et al (2002a), and Vinkó et al (2006), respectively. Schmidt et al (1994) discussed that K corrections become significant for SNe at redshifts greater than 10 4 km s −1 .…”

Section: Calibration Of the Photospheric Magnitudementioning

confidence: 99%

Photospheric Magnitude Diagrams for Type Ii Supernovae: A Promising Tool to Compute Distances

Rodríguez

Clocchiatti

Hamuy

2014

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We develop an empirical color-based standardization for Type II supernovae (SNe II), equivalent to the classical surface brightness method given in Wesselink. We calibrate this standardization using SNe II with host galaxy distances measured using Cepheids, and a well-constrained shock breakout epoch and extinction due to the host galaxy. We estimate the reddening with an analysis of the B −V versus V −I color-color curves, similar to that of Natali et al. With four SNe II meeting the above requirements, we build a photospheric magnitude versus color diagram (similar to an H-R diagram) with a dispersion of 0.29 mag. We also show that when using time since shock breakout instead of color as the independent variable, the same standardization gives a dispersion of 0.09 mag. Moreover, we show that the above time-based standardization corresponds to the generalization of the standardized candle method of Hamuy & Pinto for various epochs throughout the photospheric phase. To test the new tool, we construct Hubble diagrams for different subsamples of 50 low-redshift (cz < 10 4 km s −1 ) SNe II. For 13 SNe within the Hubble flow (cz CMB > 3000 km s −1 ) and with a well-constrained shock breakout epoch we obtain values of 68-69 km s −1 Mpc −1 for the Hubble constant and a mean intrinsic scatter of 0.12 mag or 6% in relative distances.

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The first year of SN 2004dj in NGC 2403★

Cited by 61 publications

References 49 publications

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj

THINGS about MOND

Photospheric Magnitude Diagrams for Type Ii Supernovae: A Promising Tool to Compute Distances

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