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The total number of Primary Orbits used in all Cycles must equal the total number of Primary Orbits specified on all the Observations. (Compare totals reported on the first and second pages of the PDF Preview.)
Small GO Proposals are not allowed in Cycle 26 unless they are Joint Programs.
Please specify your scheduling constraints or 'No Constraints' on all Observation forms.0Assigned ID: 610
----- Attempting Submission 1 (Tue Nov 27 14:51:13 GMT 2018) -----Joint NRAO/HSTORBITAL VISIBILITY OVERRUNVersion 4: Resubmitted for 2 orbits of observations after the faliur of the first observations.
Version 3 changes:.
1. We improved the coordinates to RA=15:12:25.1, Dec=+01:29:54.20 and the uncertainty to 0.4" based on a detailed study of the GALEX image.
2. We also an addition exposure. We are now performing ACQ/SEARCH and then ACQ/IMAGE, to improve the positional accuracy of the UV source.
3. We also corrected the COS ETC ID in the exposures COS.sp.1178547.1927741871----- Attempting Submission 1 (Tue Jan 08 16:39:33 GMT 2019) -----
HST Phase II Proposal 15666 (APT_2.apt) successfully submitted.
Receipt: # 15666-1
----- Attempting Submission 2 (Tue Jan 08 16:40:37 GMT 2019) -----
HST Phase II Proposal 15666 (APT_2.apt) successfully submitted.
Receipt: # 15666-2
----- Attempting Submission 3 (Fri Feb 15 05:00:36 GMT 2019) -----
HST Phase II Proposal 15666 (APT_2.apt) successfully submitted.
Receipt: # 15666-3
----- Attempting Submission 4 (Thu Jul 04 19:17:17 GMT 2019) -----Visit 1 has warmings. These observations failed so they are not applicable. I am not able to remove them from the file so they are still there.Probing Infall of Cold Gas in an Interacting GalaxyThe inflow of massive amounts of gas towards the centers of galaxies is commonly seen in simulations of galaxy interactions and mergers. Such inflows are associated with strong starbursts in interacting galaxies as well as their enhanced nuclear activity. While the importance of inflow of gas is clear, there is little observational data to strengthen our understanding of the physics of gas inflow. This program aims to study a rare case where our previous D- and C- configuration VLA imaging detected blue-shifted HI 21cm emission tracing infall of atomic gas into a spiral galaxy. We request for 27.5 hours of high-resolution VLA B-configuration imaging to identify the location of the inflowing gas and to characterize its nature and origin. We also request for 3 orbits of ultraviolet spectroscopy with HST COS to establish the origin of the gas as inflow and rule out outflow with high confidence. This system is truly unique and provides unprecedented opportunity to study infall of gas into galaxies that have so far been studied only in simulations. Therefore, we believe that our modest request of 27.5 hours of the VLA and 3 orbits of the HST will yield significant scientific results.The main goals of this project are to (1) confirm if there in ongoing infall of gas into the target galaxy and (2) if so, reveal the physical process responsible for it.
The program aims to obtain UV spectrum with G130M. The spectrum will be analyzed to estimate outflow signatures (at 200 km/s centroid) and to verify inflow. In addition to the standard target acquisition image, we will obtain deeper NUV images with MIRRORA along with the spectroscopic observations. These images will provide important guidance for the interpretation of the spectra. The high-angular resolution of COS NUV imaging (47.1 mas/resel) is a factor of > 120 higher resolution than existing GALEX NUV imaging (where the source is unresolved). The data will be complemented by ground-based imagery and would link the connection between location of gas inflow and recent star-formation.
A detailed study of the COS UV spectra and comparison of Starburst99 models will be used to predict the stellar populations (age, burst type etc.). The nature of the ISM combined with morphology of star forming region will provide vital clues about the triggering mechanism of star-formation in an interacting system. We will interpret our data and measurements in terms of results from simulations.
We require 3 orbits to get a COS spectrum with G130M granting in the 1327 setting. The galaxy has a FUV GALEX magnitude of 18.3. Based on the u-band size in the SDSS image, we expect the UV magnitude within the COS aperture to be from 18.3 -19.0 mag. Based on that we request for 3 orbits to get a S/N of 10 at 1251A so that we can cover Lyman-alpha, Si II 1260, 1190, 1193, OI 1302 and multiple other species at a S/N ~10. The ETC IDs for these calculations are COS.sp.1178547 and COS.sp.1178545.Galaxies and the IGM6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYINTERACTING GALAXYNOJ2000J2000GALEX FUV=18.3 & NUV=17.9COS/FUVSpectroscopicNoNoG130M1327The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode./Users/Sanch/Dropbox (ASU)/Inflow/APT/OP-cache/APT_15666_Inflow-v01.xml3 orbits1558183752000180.66890491131744(Tic-Visit
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