The following comments still apply for resubmittion of this proposal #981:
I am sorry for the inconvenient, but this is a resubmission of proposal 86, originally titled
"Are the most isolated dSph galaxies truly old?" PI Matteo Monelli.
The original submitted .apt was deleted by mistake, and I had to generate a new one.
Please withdraw the previous submission.
Matteo Monelli-2046898574Assigned ID: 981
----- Attempting Submission 1 (Fri Apr 07 22:12:37 GMT 2017) -----
HST Phase I Proposal 981 (monelli_isolated_c25.apt) successfully submitted.
Receipt: # 981-1
----- Attempting Submission 2 (Fri Apr 07 22:16:27 GMT 2017) -----
HST Phase I Proposal 981 (monelli_isolated_c25.apt) successfully submitted.
Receipt: # 981-2The proposal targets the RR Lyrae star population of two galaxies at the fringes of the Local Group.
The current observing strategy is based on successfull previous HST projects. As the target stars are faint (V~26.5) we set the longest possible individual exposure per orbit.
In the case of one galaxy, KKr25, the poiting has been optimized to avoid the contamination of nearby bright field stars.
This is a resubmission on Jan 17, 2019, after the approval of HOPR 91467 to repeat two failed orbits fro visit 1 and 2.342576412----- Attempting Submission 1 (Wed Jul 19 14:12:47 GMT 2017) -----
HST Phase II Proposal 15244 (15244.apt) successfully submitted.
Receipt: # 15244-1
----- Attempting Submission 2 (Mon Sep 11 13:33:38 GMT 2017) -----
Submission failed due to an internal error during the submission process.
If this error persists please contact the help desk at help@stsci.edu.
Submission failed due to an internal error during the submission process.
If this error persists please contact the help desk at help@stsci.edu.
Submission failed due to an internal error during the submission process.
If this error persists please contact the help desk at help@stsci.edu.
----- Attempting Submission 3 (Tue Dec 18 12:08:46 GMT 2018) -----
----- Attempting Submission 4 (Thu Jan 17 14:52:50 GMT 2019) -----A challenge to dSph formation models: are the most isolated Local Group dSph galaxies truly old?What is the origin of the different dwarf galaxy types? The classification into dwarf irregular (dIrr), spheroidal (dSph), and transition (dT) types is based on their present-day properties. However, star formation histories (SFHs) reconstructed from deep color-magnitude diagrams (CMDs) provide details on the early evolution of galaxies of all these types, and indicate only two basic evolutionary paths. One is characterized by a vigorous but brief initial star-forming event, and little or no star formation thereafter (fast evolution), and the other one by roughly continuous star formation until (nearly) the present time (slow evolution). These two paths do not map directly onto the dIrr, dT and dSph types. Thus, the present galaxy properties do not reflect their lifetime evolution. Since there are some indications that slow dwarfs were assembled in lower-density environments than fast dwarfs, Gallart et al (2015) proposed that the distinction between fast and slow dwarfs reflects the characteristic density of the environment where they formed. This scenario, and more generally scenarios where dSph galaxies formed through the interaction with a massive galaxy, are challenged by a small sample of extremely isolated dSph/dT in the outer fringes of the Local Group. This proposal targets two of these objects (VV124, KKR25) for which we will infer their SFH -- through a novel technique that combines the information from their RR Lyrae stars and deep CMDs sampling the intermediate-age population -- in order to test these scenarios. This is much less demanding on observing time than classical SFH derivation using full depth CMDs.This proposal targets two galaxies at the fringes of the Local Group, VV124 and KKr25 (16 orbits each). The main scientific objective is the detection and characterization of RR Lyrae variable stars. These are stars pulsating with period from 0.2 to 1 day.
We will adopt identical approach for both galaxies, based on successful observations in previous cycles.
1) The central region of both galaxies will be observed with the ACS in the F475W and F814W pass-bands. Coordinated parallel exposures with WFC3 are requested in the same filters to sample the outskirts of the target galaxies;
2) for each galaxy we require 8 visits of 2 orbits each;
3) we will observe one F475W and one F814W image per orbit, both with the ACS and the WFC3. The order of the filter is reversed in the second orbit of each visit, to allow larger time baseline between the shorter wavelength images, as the amplitude is larger in F475W than in F814W;
4) the total time baseline of the observation of each galaxy should not exceed few days (6 days). It has to be larger that the typical period of RR Lyrae stars, but given the relatively low number of phase points (16), periods are much better estimated is the total time coverage of the observations is short;
5) The images in the same visit are kept with the same POS TARG in order to have at least two images in the same position, which is supposed to help in the CR removal. Small ditherings are performed between visits in order to remove hot pixels and to smooth the detector response. We don't intend to cover the interchip gap. Ditherings are performed using POS-TARG, and following the basic UDF dither pattern, shifting the pointings by ~2 pix.
6) The first visit to each object is requested within a given range of orientations. Subsequent visits to each object are requested to be obtained with the same ORIENT as the first visit, to maximize the sky area covered at full depth both in the prime and the parallel fields;
7) the exact pointing and ORIENT angle have been chosen according to the following criteria:
- VV124: the WFC3 coordinated field sample the outmost region of the stellar disk of VV124. This implies a relatively small range of angles of 22 degrees of both sides of the disk;
- KKr25: three bright stars are located near the main body of this galaxy. One of them (V=11.4 mag) is located within the gap, for any ORIENT angle. The selected possible range of ORIENT angles are such that a second nearby star (V=10.4 mag) does not enter for ACS field of view.Stellar Populations6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYDISKDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF SPHEROIDALThis object was generated by the targetselector and retrieved from the NED database.J2000J2000ACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF814WTiming link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08) within 6.0 days] [02 After 01 by 0.2 to 3.0 days])Hst Same orient constraint links visits (01 02 03 04 05 06 07 08 51)The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode./tmp/OPVisit16595388795317179235.xmlThis is the first visit toVV 124. We request a range in orientations in this first visit with the same orientation requested in subsequent visits to this target. This requirement will ensure that the parallel WFC3 fields of view will match exactly across all visits to this target.
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