DRAFT
2024-10-14 17:41:27
Type: Object/s-Data/Analysis
Bibcode: 2024TNSAN.296....1B
DAO photometric follow-up of selected transients (Oct. 2024 - II)
Authors: D. D. Balam (Dominion Astrophysical Observatory, National Research Council of Canada) & Eric Hess (RAO/University of Calgary)
Source Group: DAO_OTS
Keywords: Photometry
Abstract:
We present (SDSS) g&r filter photometric follow up observations of selected optical transients obtained using the 1.82-m Plaskett telescope of the (Dominion Astrophysical Observatory) National Research Council of Canada during subsequent nights of the October 2024 dark run.
SDSS filter photometry of transients
Object UT g (SDSS) g - r Presumed host z (published)
2024xqe 2024 10 13.436 16.94 (0.01) +0.44 (0.02) WISEA J022112.12+361943.4  
2024xrd 2024 10 13.374 18.04 (0.01) +0.66 (0.02) SDSS J011309.29+274804.5 0.073 p
2024xsv 2024 10 13.242 19.97 (0.08) -0.11 (0.11) WISEA J220359.16+364942.4  
2024xtb 2024 10 13.180 20.43 (0.08) +1.50 (0.09) SDSS J215721.05+265050.7 0.122 p
2024xtt 2024 10 13.305 18.96 (0.02) +0.40 (0.03) SDSS J234618.58+290640.8 0.075 p
2024xvg 2024 10 13.11 18.10 (0.01) -0.06 (0.02) WISEA J191544.81+441035.6  

Photometric observations obtained with the 1.82-m Plaskett telescope are differential (SDSS gri filters) and measured from stars in either the Sloan Digital Sky Survey (Skyserver) or the Pan-STARRS release 1 (PS1) Survey - DR1.

The transient host galaxy light in our photometric measurement is minimized via one of two methods: Reference images are downloaded from the PanSTARRS image access (Flewelling, H. A., et al.) and are convolved, using the nightly PSF to match our images. The reference is then subtracted from our co-added images. A secondary photometric standard is defined and retained on the subtracted image using a pixel mask. 

A second method involves creating a model galaxy, using the IRAF artdata packages, scaling it to the images and subtracting the host galaxy. The differential photometry  was then performed using Image Reduction and Analysis Facility (IRAF) (Tody, D. 1986, "The IRAF Data Reduction and Analysis System").

Note:  photometric redshifts are marked 'p' and spectroscopic redshifts are marked 's'. All host redshifts are via the SDSS Skyserver.

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 2024xqe 02:21:11.941 +36:19:48.69 02:21:11.939 +36:19:48.60 SN Ia 0.034
TNS 2024xrd 01:13:09.360 +27:48:08.20 01:13:09.360 +27:48:08.20 SN Ia 0.0452379
TNS 2024xsv 22:03:59.367 +36:49:48.49 22:03:59.367 +36:49:48.49
TNS 2024xtb 21:57:21.081 +26:50:51.22 21:57:21.081 +26:50:51.22
TNS 2024xtt 23:46:18.630 +29:06:39.65 23:46:18.630 +29:06:39.65
TNS 2024xvg 19:15:44.753 +44:10:32.26 19:15:44.753 +44:10:32.26 SN Ia 0.03

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