0 Assigned ID: 7795 ----- Attempting Submission 1 (Thu Apr 16 23:26:54 GMT 2026) ----- The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. The unique ID for this investigator was not found in the STScI database. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. I am getting an error for the STScI indeintifier in the authours list. I assume this is a bug in APT, because this was not showing up before, only when I went to actually do the submisison. The warnings have already been mentioned to IS and PC and apparently they are either bugs or can be disregarded for this proposal. 1117888389 ----- Attempting Submission 1 (Tue Aug 18 11:37:47 GMT 2026) ----- The error I am getting for the CoIs and myself appeared when I clicked to do the submission. I am not sure why it happened, but all autthors were porperly listed in Phase I. I tried doing a new search but the system is unable to find anyone. I think this is either a bug in APT of a problem of comunication to the STSci servers. Regardingthe COS warning, the FP-POS are in increasing order. I do not understand this warning. I contacted the IC and they told be to proceed with the submission. Regarding the limitations for extneded targets, this is something we already knew and it is intrinsic to our source, a galaxy. We dont expect this to be detrimental to our science as this is a compact object and we enforce a SAME ORIENT constraint, reducing the vigneting within the COS apperture. The "UV upturn" (an unexpected rise in ultraviolet flux in massive early-type galaxies) remains one of the most enduring mysteries in stellar population. Despite decades of study, it is still unclear whether this emission originates from old, evolved stars (e.g. extreme horizontal branch stars) or trace amounts of recent star formation (<1% by mass). This degeneracy is perfectly encapsulated in the massive relic galaxy NGC1277. As a unique system that has evolved in isolation since z~2 without accreting external gas or satellites, NGC1277 should be the definitive template for a purely passive stellar population. However, recent conflicting analyses of its SED and line-strengths have reached opposed conclusions: one favouring a 0.8% mass fraction of young stars, and the other a purely evolved, old UV-bright component. We propose HST STIS (NUV) and COS (FUV) spectroscopy to break this degeneracy. By measuring sensitive NUV absorption indices and FUV features, we will definitively identify the physical drivers of the UV flux. This observation will provide an unparalleled benchmark for stellar population models, determine if internal recycling can sustain star formation in the absence of mergers, and unlock the UV's potential as a probe of late-time assembly in the most massive galaxies in the Universe. This propsal aims at obtaining high quality spectra for NGC 1277 in the ultraviolet region, convering the FUV and NUV using a combination of STIS-MAMA and COS to achieve this. NGC1277 is an extended faint source in the UV (GALEX NUV = 19.713 mag; GALEX FUV = 20.446 mag). We estimate the central surface brightness to be ~19 mag arcsec^2 in the NUV and ~19.8 mag arcsec^2 in the FUV. Therefore, we would like to maximize the light-colecting time available to us focussing on spectroscopy. We estimate that an exposure time of 11 ks yields S/N~15 when integrating over the central 3'' for the STIS-MAMA observations with G230L grating, enough for our scientific needs. For the FUV observations, 20 ks are required to achieve S/N ~ 7 with the G140L grating (1105 setting). In this way, we will split our 15 HST orbits into 5 visits of 3 orbits each. 2 visits for STIS and 3 visits for COS. visits 1 and 2: STIS-MAMA orbit1: acquisition + FUV imaging + G230L exposure orbit2: G230L exposure + G230L exposure orbit3: G230L exposure + G230L exposure visits 3,4 and 5: COS orbit1: star acquisition + blind offset + NUV imaging + G140L exposure at 1105 AA FP-POS=1,2 orbit2: G140L exposure at 1105 AA FP-POS=3,4 + G140L exposure at 1105 AA FP-POS=1 orbit3: G140L exposure at 1105 AA FP-POS=2,3,4 -------------------------------------------- Acquisition For STIS, we will acquire images for the target directly. With the acquisition performed, we will center the slit and obtain long exposures using the grism obtained with COS. For COS, because the target is quite faint we would like to acquire a nearby star then use the offset to get to the galaxy. obtaining NUV imaging to check if NGC 1277 is centered. Using GAIA DR3 we selected the star GAIA DR3 239421925421815424, a relatively bright star close to NGC 1277 (~1.5' away from NGC1277). Another relatively brigth could have been used but upon inspection in GALEX images we saw that we could not dicern the origin of the emission between two stars, therefore the acquisition could be contaminated by this uncertainty. We then went GAIA DR3 239421925421815424, an F8V star (~6300 K) with G magnitude of 16.3154 mag without any apparent companion. This star is being flagged by the BOT only because it assumes the star is an O5V which produces a lot more UV radiation. That is, however, not the case. We then perform a blind offset to NGC 1277 where scince exposures will be performed. We determined the coordinated for NGC1277 both from SDSS AND ACS/WFC3 images from the HLA. ------------------------------------------- Imaging For STIS will get imaging in the FUV to help us interpret the FUV spectra. We were able to fill teh orbits allowing us to dedicate some time for the imaging without compromising the time required to get the spectra. Unfortunately STIS is less sensitive in the FUV. This exposures do not interfere with the scientific exposure but provide valuable information regarding the light ditribution of the UV bright component somethig still unknow at this spatial scales. This is pending TTRB approval. For COS, given that the apperture is smaller getting this exposure are even more important. 300s exposures will be obtained to detemine the NUV light distribution. During the images exposures, the calibration lamp should be turned on in order to align the different images from different visits. This is pending TTRB approval. --------------------------- Spectroscopy For STIS, we use only the G230L grating. This willl allow us to cover the UV and combine with ground-based data, For COS, we will use G140L grating at 1105 A finishing ht efull UV access to the source. We will use the FLASH option and all the FP-POS, as the Handbook suggests. Collectively, the team in this proposal has a lengthy background in stellar population analysis in galaxies across the electromagnetic spectrum, particularly involving NGC 1277. Dr. Anna Ferre Mateu is an expert in compact galaxies and star-formation history retrieval, and among the first to point out the relic nature of NGC 1277. Dr. Alexandre Vazdekis has a vast experience in stellar population modelling, being the PI of the MILES stellar population models extension into the UV fed by HST-based libraries, using ultraviolet spectroscopy to point out the presence of young stars in old galaxies. Dr. Fabio Ditrani has several papers devoted to retrieving stellar population properties in the ultraviolet as well as implementing novel spectral analysis techniques. Dr. Ignacio Martin Navarro is an expert in detailed stellar population analysis, responsible for studying the radial stellar population properties of NGC 1277. Mr. Eduardo Hartmann recently published a letter connecting high-z quenched galaxies to NGC 1277, further evidencing its relic nature. He is a PhD student under the supervision of Dr. Ignacio Martin-Navarro. Dr. Mike Beasley is an expert in globular clusters and galaxy evolution, having used HST/ACS data in a seminal paper, showing that NGC 1277 hosts a single globular cluster population. Dr. Elham Eftekhari is a leading figure in the near-infrared analysis of stellar populations, particularly responsible for the detection of deep CO bands in NGC 1277. Mr. Joao Pedro Verardo Benedetti is a PhD student under the supervision of Dr. Anna Ferre-Mateu and Dr. Alexandre Vazdekis, studying the ultraviolet properties of early-type galaxies and their late-time build-up, with experience in stellar population analysis and spectroscopic data reduction, especially in the ultraviolet. Galaxies Stellar Populations and the Interstellar Medium 6 false true false false false false false SUPPORTED GALAXY ELLIPTICAL YES This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. This object has been oberved with HST (ACS). We checked the coordinated and they match the object center. V-band magnitude is given in mag/arcsec2 converted from the RC3 catalogue (de Vaucouleurs+ 1991). GALEX magnitudes are integrated magnitudes from 2012GASC..C...0000S. J2000 J2000 GALEX NUV = 19.713 mag; GALEX FUV = 20.446 mag STAR G III-I NO This object was generated by the targetselector and retrieved from the 2MASS database. NGC-1277-STAR J2000 Gaia Gmag 16.315447 mag GALAXY ELLIPTICAL YES This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM. GALEX NUV = 19.713 mag; GALEX FUV = 20.446 mag STIS/NUV-MAMA Spectroscopic No No G230L 2376 COS/FUV Spectroscopic No No G140L 1105 1786967928547 /home/jbenedetti/PhD_project/Proposals/27A/NGC1277/APT_PhaseII/OP-cache/HST_NGC1277-v01.xml The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. This visits primarily aims to get NUV spectra of NGC 1277 using STIS-MAMA detectors. We will use a low-disperion grating and a rather wide slit to due to the internal velocity dispersion from teh object. We will also get FUV imaging as COS acquisition is only performed in the NUV. In this way we get both NUV and FUV photometric observations aiding the interpretation of the spectral signatures. (Tic-Visit :proposal-id 18353 :visit-id "01" :proposal-version -1 :trans-version "20260618" :date "17-Aug-2026 12:58:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 817952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18353 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18353 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 339 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "01" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2617 :al-overhead-at-end 0 :internal-dur-at-end 339 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "01" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2617 :al-overhead-at-end 0 :internal-dur-at-end 601 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 Using the STIS Target Acquisition Simulator and an ACS image which has roughly the same pixel scale size as STIS ACQ (0.05 arcsec). According to the software, the minimum value for the CHECKBOX that stabilizes the centroid found is 11. For the ETC computation, we use the average surface brightness within 3 arsec for NGC 1277 (17.7 mag/arcsec2). We round the number to be 1 min exposure. Despite being a galaxy with a really concentrated bightness profile, the peak surface magnitude in the central region (~12mag/arcsec2) does not saturate the detector. Given that COS does not allow for FUV imaging, we decided to get STIS exposures in the FUV to help us interpret the spectra without compormising the integration time required for the spectrosopic observations. Using the GALEX integrated magnitudes we estimated the averange surface magnitude in the FUV to be 20.37 mac/arcsec2 in the inner 2 arcsecs where we expect to detect most of the FUV flux. Given that we have two visits, we will be able to get 2 image exposures for this source. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. 1786967929654 /home/jbenedetti/PhD_project/Proposals/27A/NGC1277/APT_PhaseII/OP-cache/HST_NGC1277-v02.xml The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. This visits primarily aims to get NUV spectra of NGC 1277 using STIS-MAMA detectors. We will use a low-disperion grating and a rather wide slit to due to the internal velocity dispersion from teh object. We will also get FUV imaging as COS acquisition is only performed in the NUV. In this way we get both NUV and FUV photometric observations aiding the interpretation of the spectral signatures. (Tic-Visit :proposal-id 18353 :visit-id "02" :proposal-version -1 :trans-version "20260618" :date "17-Aug-2026 12:58:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 817952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18353 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18353 :visit-id "02" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 339 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "02" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2617 :al-overhead-at-end 0 :internal-dur-at-end 339 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "02" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2617 :al-overhead-at-end 0 :internal-dur-at-end 601 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 Using the STIS Target Acquisition Simulator and an ACS image which has roughly the same pixel scale size as STIS ACQ (0.05 arcsec). According to the software, the minimum value for the CHECKBOX that stabilizes the centroid found is 11. For the ETC computation, we use the average surface brightness within 3 arsec for NGC 1277 (17.7 mag/arcsec2). We round the number to be 1 min exposure. Despite being a galaxy with a really concentrated bightness profile, the peak surface magnitude in the central region (~12mag/arcsec2) does not saturate the detector. Given that COS does not allow for FUV imaging, we decided to get STIS exposures in the FUV to help us interpret the spectra without compormising the integration time required for the spectrosopic observations. Using the GALEX integrated magnitudes we estimated the averange surface magnitude in the FUV to be 20.37 mac/arcsec2 in the inner 2 arcsecs where we expect to detect most of the FUV flux. Given that we have two visits, we will be able to get 2 image exposures for this source. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. The spectroscopic observations have been planned using the GALEX ingetrated photometry and morphological paramters for the source. We estimate that to get good quality spectra we need 11ks for NUV observations. Summing the two visits, these will be 10 exposures. We decided to do manual wavelegth calibrations exposures because the AUTO WAVECAL was placing the WAVECALS in ht emidle of the orbit given that they could happen during occultation, maximising the availabel time for the sience exposures. 1786967931279 /home/jbenedetti/PhD_project/Proposals/27A/NGC1277/APT_PhaseII/OP-cache/HST_NGC1277-v03.xml Hst Same orient constraint links visits (03 04 05) The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. This visit primarily focusses on getting FUV spectra for the galaxy NGC 1277. The acquisition strategy is a bit more intricate than for STIS due to the faintness of the source. We first acquire a star, then move the telescope to be centered in our galaxy, performing a NUV image to chech if it was properly centered. We then move on to get the spectra. These have been organized into two exposures using FP-POS=ALL, resulting in eight sub exposures two of them grouped in the first orbit and the next ones the two subsequent orbits. (Tic-Visit :proposal-id 18353 :visit-id "03" :proposal-version -1 :trans-version "20260618" :date "17-Aug-2026 12:58:51.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1487232 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18353 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18353 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2621 :al-overhead-at-end 0 :internal-dur-at-end 143 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "03" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "03" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 423 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 We got a star to anchor the positioning of NGC1277 given that it is a faint target. This is a star observed in GAIA with a spectral type F8V 6250 K. COS ETC requires 30s to acquire the target. These star is being falgged and a Health/Safety but only because in the GSC2 it assumes the star is an O5V. As previously said, this is not true and observations are safe to be conducted using COS. After the star acquisition and offset applied, we get NUV image for NGC1277 to help aid the interpretaion of the spectroscopic observations. We estiamte 300s to be enough to check if the galaxy is well centered in the apperture. We decidede to use the FLASH=YES option to get a fixed point in the detector allowing us to sum all the exposures getting an even better image. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration. 1786967932624 /home/jbenedetti/PhD_project/Proposals/27A/NGC1277/APT_PhaseII/OP-cache/HST_NGC1277-v04.xml Hst Same orient constraint links visits (03 04 05) The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. This visit primarily focusses on getting FUV spectra for the galaxy NGC 1277. The acquisition strategy is a bit more intricate than for STIS due to the faintness of the source. We first acquire a star, then move the telescope to be centered in our galaxy, performing a NUV image to chech if it was properly centered. We then move on to get the spectra. These have been organized into two exposures using FP-POS=ALL, resulting in eight sub exposures two of them grouped in the first orbit and the next ones the two subsequent orbits. (Tic-Visit :proposal-id 18353 :visit-id "04" :proposal-version -1 :trans-version "20260618" :date "17-Aug-2026 12:58:52.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1487232 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18353 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18353 :visit-id "04" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2621 :al-overhead-at-end 0 :internal-dur-at-end 143 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "04" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "04" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 423 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 We got a star to anchor the positioning of NGC1277 given that it is a faint target. This is a star observed in GAIA with a spectral type F8V 6250 K. COS ETC requires 30s to acquire the target. These star is being falgged and a Health/Safety but only because in the GSC2 it assumes the star is an O5V. As previously said, this is not true and observations are safe to be conducted using COS. After the star acquisition and offset applied, we get NUV image for NGC1277 to help aid the interpretaion of the spectroscopic observations. We estiamte 300s to be enough to check if the galaxy is well centered in the apperture. We decidede to use the FLASH=YES option to get a fixed point in the detector allowing us to sum all the exposures getting an even better image. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration. 1786967933974 /home/jbenedetti/PhD_project/Proposals/27A/NGC1277/APT_PhaseII/OP-cache/HST_NGC1277-v05.xml Hst Same orient constraint links visits (03 04 05) The scheduling data was generated by CASM 34.2. CASM was run in Phase II mode. This visit primarily focusses on getting FUV spectra for the galaxy NGC 1277. The acquisition strategy is a bit more intricate than for STIS due to the faintness of the source. We first acquire a star, then move the telescope to be centered in our galaxy, performing a NUV image to chech if it was properly centered. We then move on to get the spectra. These have been organized into two exposures using FP-POS=ALL, resulting in eight sub exposures two of them grouped in the first orbit and the next ones the two subsequent orbits. (Tic-Visit :proposal-id 18353 :visit-id "05" :proposal-version -1 :trans-version "20260618" :date "17-Aug-2026 12:58:53.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1487232 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18353 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18353 :visit-id "05" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2621 :al-overhead-at-end 0 :internal-dur-at-end 143 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "05" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18353 :visit-id "05" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2619 :al-overhead-at-end 0 :internal-dur-at-end 423 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 We got a star to anchor the positioning of NGC1277 given that it is a faint target. This is a star observed in GAIA with a spectral type F8V 6250 K. COS ETC requires 30s to acquire the target. These star is being falgged and a Health/Safety but only because in the GSC2 it assumes the star is an O5V. As previously said, this is not true and observations are safe to be conducted using COS. After the star acquisition and offset applied, we get NUV image for NGC1277 to help aid the interpretaion of the spectroscopic observations. We estiamte 300s to be enough to check if the galaxy is well centered in the apperture. We decidede to use the FLASH=YES option to get a fixed point in the detector allowing us to sum all the exposures getting an even better image. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration. This is the exposures to get the FUV spectrum once the object has been properly placed in the apperture. We estiamte we need 17ks for this. We organized for each of the three visits two exposures using all FP-POS, resulting in 24 sub exposures. This exposure streches accross two orbits. We decide to use the FLASH=YES to allow for time-resolved wavelegth calibration.