SDSS filter photometry of transients
|
Object |
UT |
g (SDSS) |
g-r |
Presumed host |
z (published) |
|
2024nvo |
2024 07 06.253 |
17.41 (0.01 ) |
+0.75 (0.02) |
SDSS J144424.28+383919.5 |
0.106 p |
|
2024nvi |
2024 07 06.315 |
20.42 (0.05) |
+0.86 (0.05) |
SDSS J165358.59+302000.9 |
0.277 p |
|
2024nkl |
2024 07 06.377 |
19.68 (0.05) |
------- |
SDSS J173000.69+254900.4 |
0.072 p |
|
2024nut |
2024 07 08.253 |
18.40 (0.01) |
+0.05 (0.03) |
SDSS J154552.81+150741.0 |
0.160 p |
|
2024nzf |
2024 07 08.315 |
18.43 (0.01) |
+0.47 (0.02) |
SDSS J163952.93+294714.6 |
0.128 p |
|
2024nxg |
2024 07 08.377 |
18.18 (0.01) |
+0.17 (0.02) |
SDSS J170949.19+321757.1 |
0.063 s |
|
2024nxi |
2024 07 08.441 |
19.45 (0.05) |
------- |
------------- |
----- |
|
2024ozg |
2024 07 09.252 |
20.44 (0.07) |
+0.46 (0.07) |
SDSS J172935.77+355045.2 |
0.258 p |
|
2024ozx |
2024 07 09.312 |
18.19 (0.01) |
+0.56 (0.02) |
WISEA J185935.75+331804.2 |
0.064 s |
|
2024ozr |
2024 07 09.374 |
18.25 (0.01) |
+0.23 (0.02) |
SDSS J210619.40+021009.0 |
0.072 p |
|
2024ozn |
2024 07 09.437 |
18.77 (0.01) |
+0.36 (0.02) |
SDSS J223859.98+243706.4 |
0.049 p |
|
2024pdi |
2024 07 10.377 |
19.88 (0.02) |
-------- |
WISEA J190701.98+363637.8 |
----- |
|
2024pen |
2024 07 11.382 |
17.99 (0.01) |
+0.20 (0.02) |
WISEA J193046.57+405152.3 |
----- |
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.
| 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 | 2024nvo | 14:44:24.252 | +38:39:19.74 | 14:44:24.252 | +38:39:19.74 | |||||||
| TNS | 2024nvi | 16:53:58.596 | +30:20:00.83 | 16:53:58.596 | +30:20:00.83 | |||||||
| TNS | 2024nkl | 17:30:00.402 | +25:49:01.56 | 17:30:00.402 | +25:49:01.56 | |||||||
| TNS | 2024nut | 15:45:52.960 | +15:07:43.50 | SN Ibn | 0.08 | 15:45:52.960 | +15:07:43.50 | SN Ibn | 0.08 | |||
| TNS | 2024nzf | 16:39:53.018 | +29:47:14.11 | SN Ia | 0.12 | 16:39:53.018 | +29:47:14.11 | SN Ia | 0.12 | |||
| TNS | 2024nxg | 17:09:49.166 | +32:17:53.04 | SN Ia | 0.063111 | 17:09:49.166 | +32:17:53.04 | SN Ia | 0.063111 | |||
| TNS | 2024nxi | 20:50:15.394 | +31:41:52.83 | 20:50:15.394 | +31:41:52.83 | |||||||
| TNS | 2024ozg | 17:29:36.005 | +35:50:45.64 | 17:29:36.005 | +35:50:45.64 | |||||||
| TNS | 2024ozx | 18:59:35.999 | +33:18:06.77 | SN Ia | 0.068 | 18:59:35.999 | +33:18:06.77 | SN Ia | 0.068 | |||
| TNS | 2024ozr | 21:06:19.635 | +02:10:09.21 | SN II | 0.062 | 21:06:19.635 | +02:10:09.21 | SN II | 0.062 | |||
| TNS | 2024ozn | 22:39:00.444 | +24:37:37.17 | SN Ia | 0.050021 | 22:39:00.444 | +24:37:37.17 | SN Ia | 0.050021 | |||
| TNS | 2024pdi | 19:07:01.980 | +36:36:38.13 | 19:07:01.980 | +36:36:38.13 | |||||||
| TNS | 2024pen | 19:30:46.589 | +40:51:52.36 | 19:30:46.589 | +40:51:52.36 |
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