# Summary Using the Hubble Law, determine the absolute magnitudes of Type 1a supernovae occurring in distant galaxies. Background

 Дата канвертавання 21.04.2016 Памер 26.34 Kb.
Absolute Magnitudes of Supernovae

Summary Using the Hubble Law, determine the absolute magnitudes of Type 1a supernovae occurring in distant galaxies.

Background - During a three-week period in 1997, the Hubble Space Telescope was used to observe a supernova - an exploding star in a distance galaxy. These exploding stars are seen to appear suddenly, as they increase rapidly in brightness, and then to fade slowly over weeks or months. The fuzzy red object that appears at constant brightness in each of the six frames in this image is a distant galaxy, and the bright spot that is visible in the first frame in the upper left is the supernova, which gradually fades away.

On the accompanying pages are the light curves of nine Type 1a supernovae that appear in galaxies during the years 1994-1996 (Type 1a supernovae are a particular type of exploding star that contains no hydrogen lines in its spectrum). The units on the abscissa are days, and on the ordinate are apparent magnitude. Each supernova was monitored for several weeks so that its rise to maximum light and its subsequent decline in brightness were well-determined. For each, the apparent magnitude at which the supernova was brightest can be determined from the light curve. Our goal is to determine the absolute magnitude of each supernova.

Record the brightest magnitude reached for each supernova in the table below.

The recession velocities of the host galaxy of each supernova was measured from the redshift of spectral lines. The recession velocity must be measured from the host galaxy, rather than from the supernova itself, because the gas from which the supernova spectrum arises is expanding explosively from the original supernova progenitor.

Use the value of the Hubble Law to compute the distance of the host galaxy (and the supernova) from the recession velocity. Remember that the distance = velocity / Ho.

Now you can calculate the absolute magnitude from the distance and the apparent magnitude using the inverse square law. Recall that the distance in parsecs is related to the difference between the absolute and apparent magnitude as follows:

Distance in parsecs = 10(m-M+5)/5

In this case, we know the distance and apparent magnitude and want to determine the absolute magnitude. The expression can be rewritten as

M = m – 5 log(distance) + 5
 Supernova Host Galaxy z Recession velocity (km s-1) Distance in Mpc for Ho=72 km s-1 Mpc-1 App Mag (mmax) Absolute Magnitude (M) 1994S NGC 4495 0.01610 4,463 14.8 1995D NGC 2962 0.00655 1,998 1994ae NGC 3370 0.06700 1,279 1995al NGC 3021 0.00514 1,536 1995ac Anon 0.04900 14,615 1995bd UGC 3151 0.01520 4,758 1996X NGC 5061 0.00681 2,034 1996bl Anon 0.3480 10,598 1996bo NGC 673 0.01650 5.063 Average Absolute Magnitude Median Absolute Magnitude

What can you conclude about the absolute magnitudes of Type 1a supernovae?

What is peculiar about the supernova 1995bd? What explanation might account for its difference from other Type 1a supernovae?

How might your conclusions about Type Ia supernovae be useful for determining the distances to other galaxies?

This exercise is based on one developed by Lindsay Clark (see http://www.astro.princeton.edu/~clark/SNLab.html), and has been revised for use in the "Exploring the Dark Universe" workshop for teachers at Indiana University. The original data used in the exercise were obtained from Riess et al. 1999, AJ, 117, 707.

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