Submission failed communicating with the submission server:
java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is:
java.net.ConnectException: Operation timed out
Submission failed communicating with the submission server:
java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is:
java.net.ConnectException: Operation timed out
Submission failed communicating with the submission server:
java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is:
java.net.ConnectException: Operation timed out
Assigned ID: 746
----- Attempting Submission 1 (Fri Feb 24 21:44:14 GMT 2012) -----
HST Phase I Proposal 746 (wind20_v5.apt) successfully submitted.Coordinates of Target 1 (IC1613-A13) and target 2 (IC1613-B11) revised----- Attempting Submission 1 (Tue Jul 10 00:20:02 GMT 2012) -----
HST Phase II Proposal 12867 (go12867.apt) successfully submitted.
----- Attempting Submission 2 (Mon Nov 19 15:20:59 GMT 2012) -----We use single FP-POS for each individual TTAG exposure because of the limited SNR (5 to 10 ) of
each individual exposure, and because we will co-add different exposures obtained at different
central wavelenghts (beating down the FP noise this way).The Wind of Massive Stars in Low-Metallicity GalaxiesThe ultimate fate of massive stars rests on the mass and angular momentum that they loose during their evolution, hence depends on the properties of their winds. Because of the radiation-driven nature of these winds, we expect the mass loss rates to scale with stellar metallicity. Such a relation has been established theoretically and empirically with spectroscopic analyses of O stars in the Galaxy (Z/Zsun=1) and in the LMC and SMC (Z/Zsun = 1/2 and 1/5).
Tramper et al. (2011) derived mass loss rates of 6 O stars in galaxies with low metallicities (Z/Zsun ~ 1/7). Based on the Halpha line, they derived mass loss rates that are similar to those of LMC stars. This result, if upheld, would have far-reaching consequences beyond our understanding of radiatively-driven winds, and would imply for instance a lower number of collapsars and of SN Ib and Ic in low metallicity environments, hence in the high-z Universe.
We propose to coroborate or refute Tramper et al.'s result by obtaining FUV spectra of 3 O stars in the IC 1613 and WLM galaxies with HST/COS. Because of numerous iron lines and lines sensitive to wind properties, FUV spectroscopy is the adequate tool to fully address and resolve this outstanding issue of the dependence of hot, massive star mass loss rates with metallicity. A comparison of these spectra with extant STIS or COS spectra of LMC and SMC stars will provide a direct, model-independent check of the mass loss - metallicity relation. A quantitative analysis will be carried out using our state-of-the-art NLTE unified model atmospheres calculated with the CMFGEN code to establish robustly the wind properties of low-metallicity massive stars.We propose to obtain high-resolution (R=20,000) COS FUV spectra of the 3 brightest stars from Trampler et al. (2011) study. These stars, namely A13 and B11 in IC 1613 and A11 in WLM, have magnitudes V = 19.02, 18.68, 18.40, respectively (Bresolin et al. 2006, 2007). We request to observe each target in a sequence of 6 science exposures with COS, using gratings G130M (λ1291, λ1327) and G160M (λ1577, λ1589, λ1611, λ1623). This sequence provides coverage without gap of the FUV spectrum between 1132 and 1798 A. Overlapping segments will be co-added to enhance the final SNR. Thanks to the high efficiency of COS in the FUV and little extinction toward the host galaxies (E(B-V) = 0.025 and 0.08, for IC 1613 and WLM, respectively), we can achieve a sufficient SNR in 6 HST orbits for each target (2 orbits for G130M and 4 orbits for G160M, hence each orbit is dedicated to one grating position). As individual visits should not exceed 5 orbits, we propose two visits to each target (one visit of 2 orbits for the G130M observations with two different FP-SPLIT, and one visit of 4 orbits for the G160M exposures with different FP-SPLIT). Using COS Exposure Time Calculator, assuming Kurucz models for early, or late-O stars, normalized to V and corrected for extinction, we obtain a SNR of about 15 per resolution element for the final spectra (after co-addition of all exposures recorded with each grating).
The global count rate on the detector ranges is always less than 500 ct/s with G130M and less than 200 ct/s with G160M. Count rates for the brightest pixel ranges never exceed 0.1 ct/s for G130M and is always less than 0.01 ct/s for G160M. None of the targets is known or expected to exhibit significant photometric variability. COS exposures are therefore safe in the TTAG mode. Finally, we run the BOT tool for all targets and inspect the stellar fields with Aladin. There are no bright stars at proximity of our targets that may be a safety concern for COS.HOT STARS12false0.00.0falsefalsefalsefalseSUPPORTEDEXT-STARMAIN SEQUENCE OThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000E(B-V)=0.025, Teff=47500KEXT-STARSUPERGIANT OThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000E(B-V)=0.025, Teff=31300KEXT-STARSUPERGIANT OThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000E(B-V)=0.08, Teff=30000KCOS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1623COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG160M1577COS/FUVSpectroscopicNoNoG160M1589COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1623/private/var/folders/vp/y6ls6rts0bq33t6gvs2mh3000000gn/T/OPVisit2934393937607008752.xmlTiming link suitability includes constraints ([02 After 01 by at most 21.0 days])The scheduling data was generated by CASM 20.2.CASM was run in Phase II mode.As required by APT, the visit has been set up with schedulability 100%. If the orbits when the visit is actually scheduled have a longer visibility, the stellar spectrum exposures (exp. 4 & 5) would benefit of using any possible additional time.(Tic-Visit
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