This proposal contains parallel observations with ACS. At present the orient is restricted to between 350 and 360 degrees. If this causes a scheduability problem the orient restriction can be dropped. ----- Submission 1 (Tue May 02 18:05:15 GMT 2006) ----- Phase II Proposal 10856 (sbs) successfully submitted. ----- Submission 2 (Mon May 08 15:51:56 GMT 2006) ----- Phase II Proposal 10856 (sbs) successfully submitted. ----- Submission 3 (Mon May 08 16:19:07 GMT 2006) ----- Assigned ID: 6 ----- Submission 1 (Fri Jan 06 22:05:23 GMT 2006) ----- Phase I Proposal 6 (sbs15) successfully submitted. ----- Submission 2 (Mon Jan 16 16:16:03 GMT 2006) ----- Phase I Proposal 6 (sbs15) successfully submitted. ----- Submission 3 (Fri Jan 20 18:19:31 GMT 2006) ----- ----- Submission 4 (Sat Jan 28 21:02:55 GMT 2006) ----- Delayed Negative Feedback in the Super Star Clusters of SBS0335-052E The critical unanswered question in calculations of galaxy formation and evolution is the degree of feedback from the formation of the first massive stars on subsequent evolution. Even the sign of the term is uncertain. Super Star Clusters give one very dramatic answer by forming several thousand O stars in a volume with a radius of only a few parsecs. How can that many massive stars form in such a small volume without immediate dissipation of all gas by the intense ionizing radiation from the stars? SBS0335-052E has done this, not once but at least 6 times in a region of approximately 500 parsecs in size. It has also managed to do this with the third lowest metallicity of any known galaxy. The record lowest metallicity is held by its companion SBS0335-052W. These observations are designed to test one answer to this enigma; that all of the ionizing photons are absorbed within a few hundred AU of the stars that emit them. This delays the negative feedback from photoionization and allows the formation of other stars in the immediate neighborhood who are oblivious to the massive stars nearby. This scenario predicts that both molecular and ionized gas exist within the radius of the super star clusters and that their emission should be spatially coincident. We propose to test this hypothesis with high spatial resolution NICMOS camera 2 images in the hydrogen Pa alpha and molecular hydrogen (1-0) S(1) emission lines. Spatial coincidence of the emission regions will confirm that gas within the cluster is shielded from ionizing and dissociating photons and is capable of forming new stars within this tiny region in spite of the presence of thousands of massive stars. The current burst of star formation was probably triggered by interaction with the giant spiral galaxy NGC 1376. This proposal contains parallel observations of this galaxy with the ACS WFC. Due to the intense interest in SBS0335-052 we waive all proprietary rights. The observations will then immediately compliment observations by the Great Observatories, Spitzer and ground base observatories .
The proposal takes NICMOS narrow band images in Camera 2 of the Blue Compact Dwarf galaxy SBS0335-052. It also takes parallel images with the WFC of ACS in broad band filters. The program was assigned 8 primary and 8 parallel orbits. The NICMOS Primary observations take 4 exposures in 4 different narrow band filters in each of the 8 orbits. The sampling sequences, NSAMP values and Filter cadence are the same for all 8 orbits. The strong Pa Alpha line will be in the first filter so it receives less time than the other filters. Note that the redshift of the object places the Pa Alpha line in the F190N filter rather than the F187N filter which observes rest frame Pa Alpha. To avoid rotating the individual images we have asked for the same orient for all exposures. The exposures are: F190N SampSeq = Step32 NSAMP=17 F187N SampSeq = Step64 NSAMP=20 F212N SampSeq = Step64 NSAMP=20 F215N SampSeq = Step64 NSAMP=20 This is repeated in each of the 8 orbits There is no dither pattern executed in an orbit. Overall dithering is accomplished by defining 8 different target positions, 1 for each orbit. It is understood that the dither positions will not be as accurate as in orbit dithering but the dithering is only to mitigate intrapixel sensitivity variations and does not need to be accurate. ACS WFC parallel observations: The ACS WFC parallel observations are designed to image the galaxy NGC 1376 if it does not affect the scheduability of the NICMOS observations. The target galaxy is interacting with NGC 1376 and we want to see if there are signs of disturbed morphology due to the interaction. To image the galaxy the orient must be between 350 and 360 degrees. Information from the visit planner indicates that it is possible but that it limits the scheduability. We have put in the orientation limits of 350 to 360 degrees. If this causes a problem in scheduability the orient requirement can be dropped. The ACS observations are F435W ACS/WFC 2 1000 second exposures with CR split F475W ACS/WFC 2 1000 second exposures with CR split F555W ACS/WFC 2 1000 second exposures with CR split F606W ACS/WFC 2 1000 second exposures with CR split F625W ACS/WFC 2 1000 second exposures with CR split F775W ACS/WFC 2 1000 second exposures with CR split F814W ACS/WFC 2 1000 second exposures with CR split F850LP ACS/WFC 2 1000 second exposures with CR split UNRESOLVED STELLAR POPULATIONS 0 false 0.0 false false false false false SUPPORTED GALAXY DWARF COMPACT J2000 03 37 40.8000 -05 02 38.00 J2000 GALAXY DWARF COMPACT 2nd target position for SBS0335-052 J2000 03 37 40.8000 -05 02 38.00 J2000 GALAXY DWARF COMPACT 3rd position for SBS0335-052 J2000 00 00 0.0000 +00 00 0.00 J2000 GALAXY DWARF COMPACT 4th position for SBS0335-052 J2000 00 00 0.0000 +00 00 0.00 J2000 GALAXY DWARF COMPACT 5th position for SBS0335-052 J2000 00 00 0.0000 +00 00 0.00 J2000 GALAXY DWARF COMPACT 6th position for SBS0335-052 J2000 00 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