0Assigned ID: 990
----- Attempting Submission 1 (Fri Apr 07 22:19:42 GMT 2017) -----
----- Attempting Submission 2 (Sat Apr 08 05:23:34 GMT 2017) -----Hi Shelly,
I have revised the proposal as follows:
(a) the pattern has been changed to acs-wfc-dither-line (my intent had been all along to cover
the interchip gap, but i had mistakenly chosen the mosaic pattern)
(b) the target coordinates in the previous Phase 2 were OK except for one source where I had a typo,
this has been corrected
i hope the proposal is now ready for implementation.-2109376751----- Attempting Submission 1 (Thu Jul 20 23:10:47 GMT 2017) -----
----- Attempting Submission 2 (Sun Sep 10 01:12:57 GMT 2017) -----Star-Formation in Free-Floating Evaporating Gaseous GlobulesWe propose to study the stellar embryos in select members of a newly recognized class of Free-floating
Evaporating Gaseous Globules (frEGGS) embedded in HII regions and having head-tail shapes. We discovered
two of these in the Cygnus massive star-forming region (MSFR) with HST, including one of the most
prominent members of this class (IRAS20324). Subsequent archival searches of Spitzer imaging of MSFRs
has allowed us to build a statistical sample of frEGGs. Our molecular-line observations show the
presence of dense molecular cores with total gas masses of (0.5-few) Msun in these objects, and our
radio continuum images and Halpha images (from the IPHAS survey) reveal bright photo-ionized peripheries
around these objects.
We hypothesize that frEGGs are density concentrations originating in giant molecular clouds, that, when
subject to the sculpting and compression by strong winds and UV radiation from massive stars, become
active star-forming cores. For the 4 frEGGs with HST or near-IR AO images showing young stars and
bipolar cavities produced by their jets or collimated outflows, the symmetry axis points roughly toward
the external ionizing star or star cluster - exciting new evidence for our overpressure-induced star
formation hypothesis. We propose to test this hypothesis by imaging 24 frEGGs in two nearby MSFRs that
represent different radiation-dominated environments. Using ACS imaging with filters F606W, F814W, &
F658N (Ha+[NII]), we will search for jets and outflow-excavated cavities, investigate the stellar
nurseries inside frEGGs, and determine whether the globules are generally forming multiple star systems
or small clusters, as in IRAS20324.We will image 24 frEGGs in 3 filters (F658N, F606W, F814W) using the ACS WFC. We prefer ACS to WFC3 because of ACS's
higher sensitivity in the wavelength region of interest ($\sim$0.6\micron) and larger field-of-view
($202{''}\times202{''}$ compared to $162{''}\times162{''}$) which allows us to image a larger number of objects
efficiently. We will need one orbit per each of our 12 target fields; target fields have been judiciously chosen to
include multiple objects if possible. Our time estimate is based on our prior ACS imaging of I\,20324 in the F606W and
814W filters. The IPHAS imaging (in a narrow-band H$\alpha$ filter, and broad-band $r{'}$, $i\prime$ filters) of these
objects and I\,20324 shows that they have roughly similar surface brightnesses to within a factor of 2; our selected
targets are brighter than, or have comparable brightnesses to I\,20324. The typical surface brightness for I\,20324's
tadpole body was about $3\times10^{-18}$ and $2.5\times10^{-18}$\,erg\,sec$^{-1}$\,cm$^{-2}$\,A$^{-1}$\,arcsec$^{-2}$ in
the F606W and F814W filters, respectively.
The total visual magnitudes of these structured, extended, faint objects are not useful for estimating exposure times
and have all been set to a nominal value of 18 in the cover sheet. The stars seen in the head of I\,20324 are of course
much brighter than the nebulosity. We used pairs of dithered exposures, and achieved a S/N of about 10 in total
exposure times of 11.5\,min for each filter. We will use a similar strategy for this proposal, except that we will add
one short image in each of the broad-band filters for each target field, to correct for possible saturation effects
towards the stellar sources in the tadpole heads. Conservatively assuming that the fraction of flux in the F606W filter
due to line emission in H$\alpha$ and neighbouring [NII] lines is 0.5 (this fraction is likely to be higher from
inspection of the emission line spectrum of I\,20324 in Pereira \& Miranda 2007), we will use the remainder of the
exposure time (about 15\,min) in the orbit for the F658N imaging, yielding a S/N ratio of $>$6.Stellar PhysicsStellar Populations6falsefalsefalsefalsefalsefalseSUPPORTEDISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ISMCOMETARY NEBULAEMISSION LINE NEBULAMOLECULAR CLOUDPDRSTAR FORMING REGIONYESJ2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NPOS-TARGDITHER3.034LINEfalsefalse285.29ACS-WFC-DITHER-LINE1false/tmp/OPVisit4308717965269231618.xmlThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.63.3(Tic-Visit
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