Hi Galina, Thank you for the confirmation charts. I have gone over them and I have also looked again at the whole phase II from my office, where I can work better from my laptop. I have submitted a new version with a few changes: (1) I discovered an error. The orientation requirements for visit 3 were in reality intended for visit 4. Visit 3 should have no orientation requirements. This was just a mistake on my part when inputting the data. (2) I have introduced minor coordinate shifts (a few arcseconds) for targets 2, 9, and 10 based on your charts in order to include other O stars or O star candidates in the HRC field. ----- Submission 1 (Mon May 16 08:00:43 GMT 2005) ----- Phase II Proposal 10602 (o2-3) successfully submitted. ----- Submission 2 (Mon May 23 23:13:39 GMT 2005) ----- Assigned ID: 90 ----- Submission 1 (Thu Jan 20 20:15:24 GMT 2005) ----- Phase I Proposal 90 (o2-3) successfully submitted. ----- Submission 3 (Fri Jan 21 16:19:39 GMT 2005) ----- Phase I Proposal 90 (o2-3) successfully submitted. A Complete Multiplicity Survey of Galactic O2/O3/O3.5 Stars with ACS Massive stars are preferentially formed in compact multiple systems and clusters and many of them remain spatially unresolved to date, even in our Galaxy. This has hindered the determination of the stellar upper mass limit. The lack of an accurate knowledge of the multiplicity of massive stars can also introduce biases in the calculation of the IMF at its high-mass end. We have recently used ACS/HRC to resolve HD 93129 A, the earliest O-type star known in the Galaxy, into a 55 mas binary. We propose here to extend that work into a complete multi-filter ACS imaging survey of all (20) known O2/O3/O3.5 Galactic stars to characterize the multiplicity of the most massive stars. The data will be combined with existing FGS observations to explore as large a parameter range as possible and to check for consistency. We will also derive the IMF of each system using a crowded-field photometry package and processing the data with CHORIZOS, a code that can derive stellar temperatures, extinctions, and extinction laws from multicolor photometry.
We propose observing each of the objects in our sample with a combination of ACS/HRC and ACS/WFC imaging. The observing program has been designed with the following ideas in mind: Maximizing spatial resolution in order to provide as complete a study of multiplicity as possible. Avoiding saturation in at least one exposure per filter for the same reason. Using as many filters as possible in order to calculate temperatures, extinctions, and extinction laws. Detecting stars as dim as possible down the main sequence in order to calculate the IMF. Covering an area large enough to calculate the contamination to the IMF by background stars. Rejecting cosmic rays, eliminating hot pixels, and avoiding zones not covered by the detector (HRC occulting finger, WFC interchip gap). Including nebular exposures to maximize the archival value of the data. Fitting each star into a single 2-orbit visit in order to maximize telescope efficiency. Satisfying all of the above requirements is difficult due to the overhead requirements, especially those associated with buffer dumps, but not impossible. Applying the experience learned from our previous 10205 GO program, where we fit 22 HRC exposures into a single orbit to observe HD 93129, we have used APT to try different combinations until we arrived at the one presented here: The first orbit will contain HRC exposures using six continuum filters (F220W, F250W, F330W, F435W, F550M, and F850LP) from the UV to the z band and two nebular filters (F658N and F660N, corresponding to Halpha and [N II] 6584). All filters (except F660N) will be dithered using an especially-tailored box pattern that avoids the HRC occulting finger, for a total of 29 exposures. The continuum exposure times will be kept very short in order to avoid saturation by the central object (this should be possible for all filters and targets except maybe for HD 150136 A) but long enough to reach S/N ratios of approx. 1 000 for the central object. A gain of 2 will be selected in all cases except for HD 150136 A, where a value of 4 will be used in case there is a slight saturation (note that in such a case, HRC remains better than 1% linear if one takes into account the bleeding into the nearby pixels). The HRC exposures will be used for the main goal of this program, the analysis of the multiplicity of the most massive stars. The UV filters in ACS/HRC are chosen because they provide the best spatial resolution (in terms of PSF size with reasonable sampling) available at the present time for HST. The rest are selected in order to obtain as much color information as possible (see below). The second orbit will be used with WFC exposures centered on the HRC field using the three reddest continuum filters above, F435W, F550M, and F850LP. All filters will be dithered with the standard line pattern that bridges the gap between the two WFC chips and that also allows for the rejection of cosmic rays and the elimination of hot pixels. The large overheads associated with short-exposure buffer dumps make the inclusion of short exposures impossible, so we expect that some stars will be saturated. In order to minimize the impact on the photometry, a gain of 2 will be selected for the WFC exposures, thus allowing for accurate photometry of saturated stars. Furthermore, note that the region where the brightest stars are expected and where crowding is likely to be more severe will be covered by the HRC in those same filters. We will use HD 93128 as our example for S/N calculations. We model the star using an O5~V Kurucz atmosphere with V=8.77 and $E(B-V) = 0.54$ in the ACS ETC. For the six HRC continuum filters (F220W, F250W, F330W, F435W, F550M, F850LP) we get times to saturation of 3.77, 1.52, 0.76, 0.27, 0.53, and 1.16 s, respectively. Leaving a safety margin, we set the times to 2.0, 1.0, 0.5, 0.2, 0.4, and 0.8 s for each of the 4 exposures in the dithering pattern for each filter and we adjust the nebular exposure times to fill the rest of the orbit. The central star will have a S/N ratio close to 1 000 in all filters. For other cluster members, we use as a model a B8 V with a Delta m of 6 magnitudes with respect to HD 93128 and obtained S/N ratios of 5.2, 10.0, 15.8, 46.1, 61.9, and 99.7 for the six HRC continuum filters. With respect to the WFC exposures, we are able to fit two exposures of 342 s for each of the three filters, F435W, F550M, and F850LP. Using as a model an M2 V star with a $\Delta m$ of 16 magnitudes with respect to HD 93128 (i.e., a 0.4 M$_\odot$ main-sequence star), we obtain S/N ratios of 1.9, 6.1, and 37.0, respectively. The data will be extracted using a crowded-field photometry package. Given the stability of the ACS instrumental PSF and the availability of stars with very high S/N on each field for possible corrections, we can guarantee that a high-quality PSF will be produced for each filter. A special treatment will be given for two special cases: (a) the central star itself, where a detailed manual search for close companions (that the automated package may miss) will be conducted; and (b) the saturated stars in the WFC exposures, where the counts produced by bleeding into neighboring pixels will have to be added. For the five stars (between GO 10205 and this program) observed with FGS, the results from the detailed manual search for close companions will be compared with those from that instrument in order to: (a) produce a more in-depth exploration of the Delta m-separation space and (b) test both methods for consistency. After the photometry for all stars has been obtained, the resulting data will be fed into CHORIZOS, a chi-square code for parameterized photometric modeling (Ma?z-Apell?niz 2004). The output will allow us to calculate the temperature, extinction, and extinction law on a star-by-star basis, thus producing detailed and unbiased theoretical H-R diagrams that can be compared with evolutionary tracks. HOT STARS 12 false 0.0 false false false false false SUPPORTED STAR MAIN SEQUENCE O J2000 10 43 54.3720 -59 32 57.37 J2000 STAR MAIN SEQUENCE O Coordinates offset from HD 93205 in order to include HD 93204 in the field J2000 10 44 34.7400 -59 44 15.46 J2000 STAR MAIN SEQUENCE O J2000 10 44 45.0280 -59 33 54.67 J2000 STAR OF Target coordinates correspond to a point in between MJ 257 and HD 93162 J2000 10 44 13.0000 -59 43 10.00 J2000 STELLAR CLUSTER STAR FORMING REGION OB ASSOCIATION V magnitude is that of the brightest star in the field J2000 11 15 7.1000 -61 15 38.00 J2000 STAR OF Target coordinates correspond to a point in between Pismis 24-1 and 24-17 V magnitude is that of Pismis 24-1 J2000 17 24 44.1000 -34 11 59.48 J2000 STAR MAIN SEQUENCE O J2000 07 53 38.2060 -26 14 2.62 J2000 STAR OF J2000 16 41 20.4450 -48 45 46.74 J2000 STAR OF Coordinates offset from Cyg OB2-7 in order to include Cyg OB2-17 in the field J2000 20 33 14.1120 +41 20 21.88 J2000 STAR OF Coordinates offset from Cyg OB2-22A in order to include neighbor members of Cyg OB2 in the field J2000 20 33 8.9000 +41 13 15.00 J2000 STAR OF J2000 20 17 29.7030 +37 18 31.13 J2000 STAR MAIN SEQUENCE O J2000 10 44 45.0280 -59 33 54.67 J2000 ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP ACS/HRC Imaging No No F220W ACS/HRC Imaging No No F250W ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F435W ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP ACS/HRC Imaging No No F658N ACS/HRC Imaging No No F660N ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F850LP POS-TARG DITHER 2.7 LINE 0.135 false true 90.0 4 0.0 ACS-HRC-DITHER-BOX 1 false POS-TARG DITHER 2.7 LINE false true 2 5.85 ACS-HRC-DITHER-LINE 2 false POS-TARG DITHER 3.011 LINE false false 2 85.28 ACS-WFC-DITHER-LINE 3 false Orientation requirement imposed in order to ensure continuity (lack of gaps) with HD 93129 field in program 10205. 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