On Unusual Supernova SN2002bo

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Student: Abner Zapata Sobarzo , Universidad de Concepcion Advisors: -Nicholas Suntzeff -Pablo Candia -Kevin Krisciunas. On Unusual Supernova SN2002bo. The supernova SN2002 in the NGC 3190 corresponding to unusual type Ia supernovae (SNe).
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Student: Abner Zapata Sobarzo,Universidad de Concepcion Advisors: -Nicholas Suntzeff -Pablo Candia -Kevin KrisciunasOn Unusual Supernova SN2002boThe supernova SN2002 in the NGC 3190 corresponding to unusual type Ia supernovae (SNe). The uniformity of the light curves of SNe Ia has drawn considerable attention to the potencial usefulness of these objects as cosmological standard candles.The unusual SNe Ia have light-curve shapes that are slightly different from those of normal Type Ia. These differences, although not yet completely understood, may be the key to understanding not only the physical processes of this subclass, but of all SNe Ia, and may place limits on models of Type Ia progenitors.This project goals have been to present optical (UBVRI) and infrared (JHK) light curves of the Type Ia supernova SN2002bo, from 11 days before to 144 days after the time of B-band maximum, to get the ∆m15(B) relation (Phillips 1993, Hamuy et al. 1996b; Phillips et al. 1999). This is a measure of the decay in the B-band light curve from peak to 15 days after peak.I.- IntroducctionSN2002bo in NGC 3190NGC 3193NGC 3187SN2002boThere are two main classes of SNe derivate from their spectras, Types I and II, and were stablished by Minkowski (1941). Types I SNe are defined by the absence of obvious hydrogen in their optical spectra, execpt for possible contamination from superposed H II regions. SNe II all prominently exhibt hydrogen in their spectra, yet the strength and profile of Hα line vary widely among these objects.In principle the classification can be made at any time, as long as the spectrum is of sufficiently high quality.Type Ia SNe have three subclasses kwon: Those whose early-time spectra show strong Si II (Ia), Prominent He I (Ib), or Nither Si II nor He I (Ic).II.- Supernovae TypesThe late-time spectra of SNe Ia consist of a multitude of blended emission lines of iron-group elements. Although SNe Ia, which results from the thermonuclear runaway of white dwarfs, constitute a rather homogeneus subclass, important variations in their photometric and spectroscopy properties are undeniably present. SNe Ia are exceptionally useful for cosmological studies. The key point is that luminosity correlates strongly with light-curve shape; given enough high-quality observations, the luminosity of each object can therefore be calibrated. Even the extinction can be determined reliably from observations through several filters, obviating the need to use other, much more uncertain methods such as those based on the strength of the Na I D interstellar absortion lines.The light curves of Type Ia SNe are indentified before maximum are very important, because i) the light curve can be sampled more effectively, ii) the inferred distances are better constrained by the light variation around maximum than at later phases. Their light curves can be used in order to determine distances in anlogous way to classical Cepheids. III.- Cosmological Uses of SNe Ia Independent reports was received of the discovery of a supernova in NGC 3190 by Paulo Cacella (Brazil) and Hirose et al. (Japan) on 2002 March 9. The object was reported to be 17'' East and 23'' South of the center of NGC3190.Preliminary reduction of a spectrum (range 400-780 nm) of SN2002bo, obtained on Mar. 10.04 UT, with the Asiago 1.82-m telescope, shown that it is a Type Ia supernova, about 12 days before maximum. A spectrum (range 370-750 nm), obtained by V. Hradecky on Mar. 10.25 UT, with the Mt. Hopkins 1.5-m, shown it to be a reddened and possibly peculiar Type Ia supernova well before maximum. The Si II absortion near 585 nm is unusally strong. Supernova 2002boSN2002bo SpectraComparative Spectra Type Ia SNe Most of the data have been got from YALO telescope (CTIO) and few of them have been got from 0.9-m and 1.5-m (CTIO).IV.- Data ReductionLocalPhotometric SequenceSubtracted ImageDm15(B)V.- ResultsSN2002 Light Curve (UBVRI)(B-V)obs=1.302-0.012(tv-60)Dm15(B)=1.107(B-V)o= 0.725-0.0118(tv-60)The zero reddening line of Lira (1995)Absolute magnitudes of Type Ia SNe vs. decline rate parameter Dm15(B) (Krisciunas et al. 2002el)VI.- Coming up...VII.- SummarySN2002bo 2452000+jd V B I R U Photometry Telescope345.6691 15.264 0.0128 15.797 0.0161 14.876 0.0162 14.910 0.0165 16.248 0.0803 Abner Zapata S. YALO346.6795 14.940 0.0112 15.431 0.0092 14.536 0.0122 14.582 0.0105 15.759 0.0698 Abner Zapata S. YALO350.561 14.069 0.010 14.397 0.020 13.805 0.013 13.812 0.011 14.381 0.040 Kevin Krisciunas 0.9-m350.6592 14.099 0.0099 14.484 0.0218 13.784 0.0109 13.840 0.0159 14.655 0.0506 Abner Zapata S. YALO354.6484 13.706 0.0095 14.136 0.0143 13.621 0.0096 13.556 0.0129 14.313 0.0641 Abner Zapata S. YALO358.6422 13.577 0.0125 14.126 0.0102 13.699 0.0189 13.501 0.0147 14.448 0.0859 Abner Zapata S. YALO360.648 13.638 0.040 14.127 0.047 13.749 0.030 13.508 0.030 14.351 0.055 Kevin Krisciunas 1.5-m361.656 13.659 0.040 14.205 0.040 13.784 0.030 13.488 0.030 14.412 0.055 Kevin Krisciunas 1.5-m362.6188 13.654 0.0099 14.308 0.0119 13.864 0.0116 13.574 0.0116 14.837 0.0529 Abner Zapata S. YALO366.6248 13.815 0.0137 14.658 0.0252 14.144 0.0141 13.818 0.0173 15.298 0.0482 Abner Zapata S. YALO370.5477 14.068 0.0137 15.098 0.0128 14.297 0.0164 14.047 0.0147 15.838 0.0835 Abner Zapata S. YALO373.597 14.349 0.010 15.390 0.020 14.349 0.010 14.180 0.011 15.810 0.040 Kevin Krisciunas 0.9-m376.5809 14.413 0.0145 15.758 0.0239 14.098 0.0240 14.123 0.0215 16.710 0.1022 Abner Zapata S. YALO381.5832 14.658 0.0114 16.293 0.0275 14.045 0.0125 14.237 0.0097 17.225 0.1488 Abner Zapata S. YALO385.5706 14.896 0.0269 16.587 0.0540 14.066 0.0155 14.438 0.0161 17.606 0.2439 Abner Zapata S. YALO389.5784 15.218 0.0222 16.858 0.0388 14.346 0.0128 14.745 0.0138 17.621 0.2088 Abner Zapata S. YALO390.5339 15.270 0.0194 16.875 0.0458 14.429 0.0151 14.805 0.0141 99.999 9.9990 Abner Zapata S. YALO397.4814 15.548 0.0157 17.112 0.0571 14.874 0.0136 15.169 0.0150 99.999 9.9990 Abner Zapata S. YALO400.5414 15.660 0.0153 17.147 0.0127 14.976 0.0122 15.285 0.0184 99.999 9.9990 Abner Zapata S. YALOUBVRI PhotometryTable2. Optical Photometric Sequence of SN2002bo j ub eub bv ebv vr evr vi evi345.669 0.451 0.082 0.533 0.021 0.354 0.021 0.388 0.021346.680 0.328 0.070 0.491 0.014 0.358 0.015 0.404 0.017350.561 -0.016 0.045 0.328 0.022 0.257 0.015 0.264 0.016350.659 0.171 0.055 0.385 0.024 0.259 0.019 0.315 0.015354.648 0.177 0.066 0.430 0.017 0.150 0.016 0.085 0.014358.642 0.322 0.087 0.549 0.016 0.076 0.019 -0.122 0.023360.648 0.224 0.072 0.489 0.062 0.130 0.050 -0.111 0.050361.656 0.207 0.068 0.546 0.057 0.171 0.050 -0.125 0.050362.619 0.529 0.054 0.654 0.015 0.080 0.015 -0.210 0.015366.625 0.640 0.054 0.843 0.029 -0.003 0.022 -0.329 0.020370.548 0.740 0.084 1.030 0.019 0.021 0.020 -0.229 0.021373.597 0.420 0.045 1.041 0.022 0.169 0.015 0.000 0.014376.581 0.952 0.105 1.345 0.028 0.290 0.026 0.315 0.028381.583 0.932 0.151 1.635 0.030 0.421 0.015 0.613 0.017385.571 1.019 0.250 1.691 0.060 0.458 0.031 0.830 0.031389.578 0.763 0.212 1.640 0.045 0.473 0.026 0.872 0.026390.534 83.124 9.999 1.605 0.050 0.465 0.024 0.841 0.025397.481 82.887 9.999 1.564 0.059 0.379 0.022 0.674 0.021400.541 82.852 9.999 1.487 0.020 0.375 0.024 0.684 0.020
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