| transient | UT | g (SDSS) | r (SDSS) | g - r | Secondary Standard |
| 2024gmu | 2024 04 17.467 | 18.29 (0.02) | 17.92 (0.01) | +0.37 (0.03 | SDSS J155633.23+590141.1 |
| 2024goi | 2024 04 17.443 | 18.95 (0.03) | 18.68 (0.02) | +0.27 (0.03) | SDSS J154138.08+541223.1 |
| 2024gsb | 2024 04 18.363 | 18.97 (0.02) | 18.77 (0.02) | +0.20 (0.03) | SDSS J132144.42+571130.6 |
| 2024hjy | 2024 05 02.440 | 19.77 (0.03) | 18.75 (0.02) | +1.02 (0.03) | SDSS J161152.13+124535.3 |
| 2024hlr | 2024 05 02.406 | 19.08 (0.05) | 18.14 (0.03) | +0.94 (0.03) | SDSS J151038.81+494659.4 |
| 2024hnf | 2024 05 02.336 | 18.64 (0.03) | 18.35 (0.03) | +0.29 (0.04) | SDSS J141133.10+572541.1 |
| 2024hrk | 2024 05 02.475 | 20.51 (0.09) | 20.21 (0.12) | +0.30 (0.15) | SDSS J162138.04+490456.8 |
| 2024hsw | 2024 05 03.211 | 19.48 (0.03) | 19.20 (0.03) | +0.28 (0.04) | SDSS J111507.26+662741.2 |
| 2024huw | 2024 05 03.474 | 18.90 (0.02) | 18.51 (0.02) | +0.39 (0.03) | PS 135032612218865570 |
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").
footnote:
* 2024ehs - additional Sloan filter observations were obtained yielding the following differential magnitudes: u = 17.18 (0.03) and i = 16.76 (0.03)
Several different secondary standards were used from SDSS DR16 (Ahumada+, 2020) and PS1 Survey DR1 (Chambers+, 2016) to perform differential photometry using Image Reduction and Analysis Facility.
*z values are photoZ (KD-tree method) and spectrscopic z from Sloan Digtial Sky Survey (SDSS) Sky Server. * host_g magnitudes are also derived from Sloan Digtial Sky Survey (SDSS) Sky Server.