tokens: uncertainty for our source, we carried out 2000 ray-trace simulations with MARX 5.1.0 at positions near it and at the same off-axis angle. The spectrum from the multicolor disk (MCD) fit to C1–C3 (Section 3.2 ) was assumed. 2.3. The HST Images There are two images (in two filters: F606W and F814W) taken by the HST /ACS/WFC on 2004 December 15 in the field of our X-ray source. Each image has four frames of 525 s each. As will be shown later in Section 3.1 , these images indicate that our source has a candidate host galaxy SDSS J141711.07+522540.8 (GJ1417+52 hereafter) with extent ∼4′′ and a very faint candidate optical counterpart (sGJ1417+52 hereafter) at a ∼1′′ offset from the nucleus. In order to derive their main photometric parameters, we fitted the HST /ACS/WFC images using GALFIT (Peng et al. 2010 ) with multiple Sérsic components (convolved with the PSF) for the galaxy and a PSF model for the faint optical source, which seems unresolved in these images. In order to improve the statistics, especially for the faint source sGJ1417+5, the fits used 5′′ × 5′′ (centered at the center of the galaxy) stacked images (one for each filter) from aligned and bundled 16 16 http://stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-24.pdf FLC frames. The effective PSFs 17 17 http://stsci.edu/hst/acs/documents/isrs/isr0601.pdf at the position of our source in the four frames were averaged and used to fit the stacked images. Because of dithering in the observations, different frames had different degrees of distortion at the position of our source, causing some problem in stacking them. However, we found that the fits to single frames with the corresponding PSFs gave similar results. 2.4. The Gemini Spectroscopic Observation The galaxy GJ1417+52 was observed during the night of 2013 February 8 (UT) with the Gemini Multi-Object Spectrograph (GMOS, Hook et al. 2004 ) at the Gemini North Telescope, in queue mode (program ID GN-2013A-Q-37). The data were acquired during dark time (illumination fraction 0.8%), under photometric conditions and ∼070 seeing. The 400 lines/mm ruling density grating (R400) centered at 7000 Å was used. We chose a slit of width 075 and put it through the center of the galaxy GJ1417+52 and the source sGJ1417+52 in order to obtain their spectra simultaneously. A total of four exposures of 1500 s each were obtained. Small offsets in the spectral direction (50 Å) toward the blue and the red were applied between exposures to allow for the gaps between CCDs to avoid any loss of important lines present in the spectra. Spectroscopic flats and comparison lamp (CuAr) spectra were taken after each science exposure. In addition, to derive the sensitivity function and flux calibrate the science spectrum, the spectrophotometric standard star G191B2B was observed as part of the baseline calibration provided by the observation. Because the standard star was observed on a different night (2013 March 03 UT) and under different observing conditions,
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