DRAFT
2023-07-28 07:24:23
Type: Object/s-Data/Analysis
Bibcode: 2023TNSAN.213....1G
Multiband Photometry Evolution in the First Weeks of SN 2023ixf, a possible II-L Subtype Supernova
Authors: Bianciardi G., Ciccarelli A.M., Conzo G., D'Angelo M., Ghia S., Moriconi M., Orbanić Z., Ruocco N., Sharp I., Uhlár M., Walter F
Keywords: Photometry, Supernova, Galaxy, Techniques, Methods
Abstract:
Multiband photometric observations and their evaluation to instrumental magnitudes were performed using standard Johnson-Cousins filters (B, V, Rc) as well r and g Sloan filters, and not standard ones (R, G, B, and Clear filters). These were recorded from 9 observatories and from the MicroObservatory Robotic Telescope Network. The results describe the rapid ascent towards the maximum (2.5 magnitudes about in five days in the B filter) and the slow decrease after the maximum (0.0425 +/- 0.02 magnitudes/day in the B filter). The results highlight the strong variation of the B-V colour indices during the first 50 days (from -0.20 +/- 0.02 to +0.85 +/- 0.02) and V-R (from 0 +/- 0.01 to +0.50 +/- 0.01) after the explosion, presumably corresponding to the cooling of the stellar photosphere. At 50 days after the explosion the magnitude decrease from the maximum was observed to continue where it faded by 2.5 magnitudes (B filter), thus we propose SN 2023ixf is a Type II, subtype L, supernova.

By photometric observations, at the 50th day after the explosion, the star continued the decrease in its brightness and its extent reached 2.5 magnitudes in B band from the maximum of brightness, so we can propose from our data a type II-L subtype for SN 2023ixf.

2023arXiv230705612B

Show current TNS values
Catalog Name Reported RA Reported DEC Reported Obj-Type Reported Redshift Host Name Host Redshift Remarks TNS RA TNS DEC TNS Obj-Type TNS Redshift
TNS 2023ixf 14:03:38.562 +54:18:41.94 SN IIL 0.0008 M101 14:03:38.562 +54:18:41.94 SN II 0.0008
File Comments
20230710_PLOT_VRB.jpg The rise and the decline brightness decline of SN 2023ixf . The slope of the decrease in brightness of the observed SNe is different in each color band, becoming steadily shallower as we move to redder wavelengths.

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