0Assigned ID: 902
----- Attempting Submission 1 (Fri Mar 06 23:01:41 GMT 2020) -----
HST Phase I Proposal 902 successfully submitted.
Receipt: # 902-1
----- Attempting Submission 2 (Sat Mar 07 00:12:35 GMT 2020) -----
HST Phase I Proposal 902 successfully submitted.
Receipt: # 902-2Revised ORIENT by 2.6 deg to 129.55 deg or 309.55 deg as per email.
(Previous value was 126.9 deg)-812976515----- Attempting Submission 1 (Mon Jun 29 16:55:04 GMT 2020) -----
HST Phase II Proposal 16261 successfully submitted.
Receipt: # 16261-1
----- Attempting Submission 2 (Mon Jun 29 19:26:43 GMT 2020) -----
HST Phase II Proposal 16261 successfully submitted.
Receipt: # 16261-2
----- Attempting Submission 3 (Tue Feb 02 19:32:56 GMT 2021) -----
----- Attempting Submission 4 (Fri Jan 28 22:28:57 GMT 2022) -----I've run the orbit and visit planner several times and it still says they need to be run.Mrk 71: Prototype for Catastrophic Cooling in a Green Pea AnalogThe new paradigm for extreme feedback from metal-poor, compact, super star clusters (SSCs) has superwinds suppressed due to catastrophic radiative cooling of weak winds in high-density conditions. This cooling generates strong nebular line radiation in C IV, whose spatial morphology contrasts with that of He II. We propose the first ever, nebular C IV imaging with ACS/SBC to test for these conditions in Mrk 71, a metal-poor (0.1 Z_sun), nearby starburst complex with strong evidence of suppressed superwinds. This system is a uniquely accessible, spatially resolved analog of the Lyman continuum-emitting Green Pea galaxies, a population of cosmological importance, in which suppressed superwinds appear to be relevant. We also propose STIS FUV + optical observations to identify the stellar population of the parent super star cluster Mrk 71-A, which may host very massive stars > 100 M_sun. The STIS long slit will also include a second massive cluster, Mrk 71-B, that is driving a conventional, adiabatic superbubble system; this will allow us to also calibrate classical, adiabatic feedback in this cosmologically important, low-metallicity regime.We carry out deep, C IV 1550 nebular imaging with ACS/SBC using filters F150LP and F165LP. Although these are broadband filters, the shape of their responses redward of ~1650 A is identical, allowing the difference, F150LP - F165LP, to act as a ~150 A-wide filter with an effective wavelength of ~1550 A. F165LP has lower sensitivity, but we must get similar depth. We apply the ACS BOX dither pattern to optimize spatial resolution. The ORIENT is restricted to ensure that the entire Mrk 71 complex, including the superbubble of Knot B, which extends to ~8 arcsec east of Knot A, is included. We specify the same ORIENT for all imaging exposures to optimize coadding.
We will also obtain a STIS FUV spectrum with grating G140L covering the range 1150 - 1730 A, using the 0.2 arcsec longslit, aperture 52x0.2. We orient the slit to simultaneously observe Mrk 71-A and Mrk 71-B, which are 5 arcsec apart, dithering along the slit. We do not use aperture D1 so that we can obtain both objects.
Finally, we will obtain a STIS CCD spectrum with G430L, also obtaining both Mrk 71-A and B. This will cover the range 2900 - 5700 A. We use the 52x0.2 slit as before, to ensure obtaining both objects. There are extremely bright lines, in particular [O III] 5007, so we take 3 exposures dithered along the slit. The ETC gives a time to saturation of ~1300 sec.PI Sally Oey and Sergiy Silich have expertise on massive star mechanical and radiative feedback, including numerical modeling. Both have extensive experience and established track records in advancing this field, having produced 24 and 22 papers, respectively, in this area over the last decade. Silich is a leading theorist developing the suppressed superwind models described in the text. With postdoc Will Gray, Oey developed emission-line diagnostics of the suppressed superwind model (Gray, Oey, Silich+ 2019), including C IV emission that is being tested in this program.
Matt Hayes and Goeran Oestlin have pioneered ACS/SBC FUV nebular imaging, previously done in local galaxies for Lya and O VI (Hayes, Oestlin+ 2009, 2013; Hayes, ...Oestlin+ 2016). They have a variety of expertise on LAEs and LCEs, and their radiative transfer.
Linda Smith and Claus Leitherer have expertise on massive star atmospheres and starburst spectral synthesis; and Daniela Calzetti has expertise on starburst SED modeling, and also dust scattering and absorption. These members will obtain state-of-the-art estimates of the stellar population parameters in the SSCs. Smith and Leitherer are expert STIS users, and familiar with massive star UV spectra. Bethan James has expertise with HII region UV spectroscopy and photoionization modeling. You-Hua Chu has expertise on hot gas and diffuse C IV; and Megan Reiter has expertise on PDRs and molecular gas. Anne Jaskot has expertise on Green Pea galaxies, of which Mrk 71 is a local analog.
The team has several members who have developed different nebular continuum subtraction techniques (Keenan, Oey, Jaskot, & James 2017; Hong, Calzetti+ 2014; Oestlin, Hayes+ 2014).
Oey, Hayes, Jaskot, Leitherer, and Oestlin all have published extensively on local LCE and LAE candidates. Oey, James, Jaskot, and Calzetti have specifically studied the Mrk 71 system (Oey+ 2017; Micheva+ 2017; James+ 2016).Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-MEDIUMEMISSION LINE NEBULAHII REGIONKNOTSHELLSTAR FORMING REGIONYESFUV continuum = 4 x 10^-15 erg s^-1 cm^-2 A^-1 arcsec^-2 at 1300 - 1500 A from existing FOS data.
Knot B is the object flagged by the BOT. The ETC shows that it is safe, and has F336W = 18.5.
http://etc.stsci.edu/etc/results/ACS.im.1452066/J2000J2000F336W = 18.360 +/- 0.043EXT-MEDIUMEMISSION LINE NEBULAHII REGIONKNOTSTAR FORMING REGIONYESTHIS IS A COPY OF FIXED TARGET 1, BUT ADJUSTING THE POSITION IN DEC BY 1 ARCSEC.
FUV continuum = 4 x 10^-15 erg s^-1 cm^-2 A^-1 arcsec^-2 at 1300 - 1500 A from existing FOS data.
Knot B is the object flagged by the BOT. The ETC shows that it is safe, and has F336W = 18.5.
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)
(Tic-Obset
:proposal-id 16261
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:pcs-mode "FGS"
)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
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:dark-offset NIL
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:pcs-gap 0
)true30