<=== observer ===> "CTELESCO",\ "Telesco, C. M.",\ "Space Science Laboratory",\ "NASA Marshall Space Flight Center",\ "",\ "Mail Code ES-63",\ "",\ "Huntsville AL 35812",\ "USA",\ " 1 0205 5447723",\ " 1 0205 5447754",\ "telesco@ssl.msfc.nasa.gov" <=== proposal ===> "BRN_DWFS",1,3,\ {"brown dwarfs","star formation","stellar evolution"},\ {"H. Walker","M. Wells"} <=== title ===> A Search for Brown Dwarfs as Companions to Nearby Stars <=== abstract ===> SCIENTIFIC ABSTRACT No brown dwarfs have been detected yet with certainty. The definitive detection of even one brown dwarf will have a major impact on our ideas about the evolution of stars. We propose to use ISOCAM to search for brown-dwarf companions to the nearest main-sequence stars. We will image the fields centered on these stars in two passbands in the 5-15 um spectral region which, because of the high thermal background, cannot be observed from the ground with sensitivities even close to those of which CAM is capable. These observations are aimed at the detection of brown dwarfs which are as cool as several hundred Kelvins, which is much cooler than brown dwarf candidates detectable from the ground in the low-thermal-background 1-3 um spectral region. We also propose a variety of observations with CAM and PHOT of brown- dwarf candidates observed previously from the ground. OBSERVATION SUMMARY We propose to use ISOCAM to search for brown dwarfs that are companions to known late-type main-sequence stars located within 10 pcs of the Sun. The 3 arcsec pixel field-of-view will be used to permit resolution of brown-dwarf companions as close as 15 AU to the star and to provide sufficiently large spatial coverage (1.5 arcmin) that even widely separated companions will fall within the field subtended be CAM. We will survey 43 M-dwarf stars, each with two CAM passbands for 64 seconds in each band. The microscanning AOT will be used for all observations. At 10 pcs, a 500 K brown dwarf is expected to have and 8 um flux density of about 0.4 mJy. The resultant signal-to-noise ratios in the two selected passbands (LW2 and LW10) are then expected to be in the range 4-9, which should be the worse case. We will also observe with ISOCAM and ISOPHOT a sample of eight brown-dwarf candidates discovered prior to the ISO mission. ** Please note that correct proper motions are not yet given for all objects The proper motion information will be completed a.s.a.p ** <=== scientific_justification ===> Team top 40% second 30% last 30% Autumn launch PHOT : 11220 9142 10114 Spring launch PHOT : 8424 5812 5362 WHAT IS KNOWN? The mass of a brown dwarf (BD) is so low -- < 0.08 Mo -- that the maximum central temperature it attains during formation is insufficient for the ignition of nuclear reactions in its core. However, it is thought that BDs form by the same processes of cloud fragmentation as more massive objects which ultimately become stars with nuclear-burning cores. It is their postulated origin by stellar-like cloud fragmentation that distinguishes BDs from planets; numerical simulations imply that the minimum mass of a protostellar fragment is near 0.01-0.02 Mo (Boss 1987), whereas planets, which are of lower mass, form from the circumstellar disks remaining after cloud fragmentation and collapse. Therefore, the mass range 0.01-0.08 Mo is that occupied by BDs. BDs cool from effective temperatures near 3000 K to several hundred Kelvin in 10 Gyr (see Nelson et al. 1986), radiating at IR wavelengths the energy derived from their gravitational contraction and ultimately being supported against gravity by the degenerate electron gas. The number of stars formed per mass interval (i.e., the initial mass function, IMF) increases dramatically with decreasing mass, and, while the exact form of the IMF for masses below 0.1 Mo is unknown, reasonable extrapolations of the most reasonable IMFs to lower masses imply that the Galaxy may contain large populations of BDs. Determining the IMF in the mass interval spanned by the BDs is fundemental to our understanding of low-mass stellar, sub-stellar, and planetary formation. In addition, BDs may contribute significantly to the "dark matter" inferred from its gravitational effect in our own and other galaxies and in galaxy clusters. Because BDs are expected to emit nearly all of their radiation longward of a few microns, the unprecedented capabilities of ISOCAM and ISOPHOT offer the opportunity to securely detect and understand them. OPEN PROBLEMS It is likely that BDs are common in the Galaxy and elsewhere, and yet they have been very difficult to find. Just as for stars, BDs are expected to exist as single field objects, in binaries, and in stellar clusters. So far, sensitive searches for BDs have not been carried out at wavelengths longer than a few microns. Groundbased near-IR observations can be expected to result in detections of only the hottest, and hence youngest, BDs. The typical BD is probably significantly cooler than the candidates found so far, all of which appear to have effective temperatures greater than 2000 K. The primary open problems, and currently the greatest challenges, are to find BDs and determine their properties. Once these problems are addressed, we may begin to put our understanding of the evolution of sub-stellar objects on a firm footing. WHY ISO? ISOCAM will permit for the first time with high sensitivity the search for BDs out to wavelengths significantly longer than a few microns. Detailed consideration of the spectral energy distributions expected for BDs indicate that BDs as cool as 400 K (0.01-0.02 Mo) should be detectable in at least two passbands (those near 7 and 11 um) if they are within 10 pcs of the sun; keep in mind that many of our program objects are closer than 5 pcs. With the extraordinary sensitivity of ISOCAM, even cool BDs, which probably constitute most of the BD population, may at last become accessible to observation. We propose to use ISOCAM to image the fields centered on M dwarf stars (MDs) located within 10 pcs of the Sun. We will search for BD companions to those MDs. MDs are the faintest known componants of the main sequence, and therefore it will be easier to detect a faint BD companion close to an MD than it would be to detect a BD companion associated with a more massive primary. In addition, MDs are sufficiently numerous near the sun that a reasonable sample can be defined. There is also some theoretical evidence (Boss 1987) that the stars which form in binary systems tend to be of comparable mass, so that our choice of the lowest mass main-sequence stars may positively bias our sample toward BD secondaries. We plan to use ISOCAM with the 3.0 arcsec pixel field-of-view because that configuration provides a useful balance between spatial resolution and spatial coverage. At 10 pcs, the 1.5 arcmin spatial coverage of the array corresponds to 900 AU, so that we will detect a BD located as far away as 450 AU in projection from the MD. The average projected radial separation for visual binaries is several hundred AU (see Figure 2 in Probst 1986), so that there is a reasonable probability that a BD companion will fall within the CAM field. How many BDs should we be able to discover in our 43 MD fields? Referring to the analysis by Zuckerman and Becklin (1987), we assume that half the MDs are in binary systems, half have acceptable separations from the BDs (< 450 AU), and the IMF follows a Salpeter function (admittedly a dubious assumption) below a few solar masses. We should discover about 9 BDs among our sample. We also propose to observe seven objects suspected to be BDs prior to the ISO mission. These objects are fairly bright, so that higher-spectral-resolution observations will be possible for some of them. Some of the objects are very close to the theoretical 0.8 Mo boundary between stars and BDs, and their detailed study will provide insight into the properties of that star-BD transition region. WHAT GROUNDBASED/AIRBORNE OBSERVATIONS ARE LIKELY BEFORE ISO? The major development bearing on this program will be the substantial increase in the use of detector arrays at large groundbased telescopes, especially those in the 8-to-10 meter class. Imaging at 1-5 um will continue to find higher-temperature BDs for which ISOPHOT and ISOCAM should determine the SEDs at > 5 um. Also interesting is the possibility that very sensitive arrays operating near 10 um will be able to make the first detections of much cooler BDs. It is very difficult to predict the sensitivities of these arrays, but a very naive extrapolation from current instrument performance suggests that a cool BD may be detectable at 10 um in two nights of integration with a 10 meter telescope at Mauna Kea. Given the pace of technological advance, however, it is probable that the groundbased 10 um detector systems on large telescopes will not fulfill their potential until well after the ISO mission. OBSERVING STRATEGY For our MD survey, we propose observations at 6.8 um (LW2) and 11.5 um (LW10). Those CAM bands have excellent sensitivities (typically achieving S/N = 1 for a source emitting 0.1 mJy in the survey integration time), and they span the spectral region of maximum emission anticipated for nearly all BDs. During each observation, we will center the 1.5 arcmin CAM field on each of our program MD stars. We will use the microscanning AOT for all observations in this proposal, which should be especially suitable for the detection of faint point sources. For brighter sources, this AOT should also provide a better data set for super-resolution analyses. The strategy to be taken for the seven known BD candidates will differ among the objects, depending on source brightness and multiplicity. For several of these objects, higher spectral resolution observations will be made in an attempt to search for absorption features diagnostic of a cool BD photosphere (Lunine 1986). The 43 M dwarfs that we propose to observe in our survey are listed in Table 1. The first 24 objects (left side of table) are from the list of Henry and McCarthy (1990) and constitute all known MDs within about 5 pcs and at Dec > -30 deg; that Dec limit is useful for permitting preparatory and follow-up observations of each object. Using speckle interferometry at 2 um, Henry and McCarthy searched unsuccessfully for low-mass companions closer than a few arcsecs to each of these MDs. Our search will substantially extend their study to much greater radii and much longer wavelengths. The last 19 entries in Table 1 (right side of table) are from the list of Skrutskie et al. (1989), and all are within 10 pcs of the Sun. Using an array at 2 um, Skrutskie et al. searched a 14 arcsec field centered on each of these stars for low-mass companions, thereby discovering GL 569 (their only BD candidate) which we propose to observe as part of the current program with ISO (see below). Again, our proposed observations of the Skrutskie et al. sample will employ a much greater FOV and vastly extended wavelength coverage. The eight previously discovered BD candidates for which we propose more detailed observations are listed in Table 2. Total integration times for each object are also given in the table. The proposed observations differ among the sample, depending on known or estimated source properties. Both ISOCAM and ISOPHOT are proposed for these observations. This sample constitutes nearly all of the objects currently considered to be possible BDs (see, e.g., Henry and McCarthy 1990). Note that when CAM is used for these observations, the PFOV will be 1.5 arcsec, in contrast to the MD survey use of CAM for which the PFOV will be 3.0 arcsec. Field coverage is not important for the BD candidates; we prefer having the higher spatial resolution, which will facilitate resolution boosting where feasible. M dwarfs in the Orion hole are flagged with a double asterisk in Table 1, and those in the Galactic Center hole are flagged with a single asterisk. Table 1. M Dwarfs to be Searched for Cool Companions Gliese RA Dec D Gliese RA Dec D Number H M S D M S pcs Number H M S D M S pcs 1002 00 04 13 -07 47 30 4.7 35 00 46 31 +05 09 12 4.2 15 00 15 31 +43 44 24 3.4 65AB 01 36 25 -18 12 42 2.7 54.1 01 09 59 -17 16 24 3.8 555 14 31 35 -12 18 36 6.3 83.1 01 57 28 +12 50 06 4.5 638 *16 43 15 +33 35 42 9.6 166C 04 13 04 -07 44 06 4.8 644 *16 52 48 -08 14 42 6.4 273 **07 24 43 +05 22 42 3.8 654 *17 02 37 -05 00 42 9.9 1111 08 26 53 +26 57 12 3.6 655 *17 05 01 +21 37 06 9.8 388 09 16 54 +20 07 18 4.9 694 *17 42 25 +43 24 24 9.7 LHS292 10 45 41 -11 03 06 4.6 695 *17 44 28 +27 44 42 7.8 406 10 54 06 +07 19 12 2.4 799 20 38 44 -32 36 36 8.2 411 11 00 37 +36 18 18 2.5 803 20 42 04 -31 31 06 9.3 445 11 44 35 +78 57 42 5.2 829 21 27 12 +17 25 06 6.5 447 11 45 09 +01 06 00 3.4 831 21 28 34 -10 00 36 7.5 526 13 43 12 +15 09 42 5.2 846 21 59 39 +01 09 42 9.5 628 *16 27 31 -12 32 18 4.0 849 22 07 00 -04 53 12 8.9 687 17 36 42 +68 23 06 4.7 852 22 14 42 -09 03 00 9.6 699 *17 55 23 +04 33 18 1.8 867 22 36 01 -20 52 48 9.2 725 18 42 12 +59 33 18 3.5 880 22 54 10 +16 17 24 6.8 729 *18 46 45 -23 53 30 2.9 896AB 23 29 20 +19 39 42 6.5 1245 19 52 16 +44 17 30 4.7 866A 22 35 45 -15 35 30 3.4 873 22 44 40 +44 04 24 5.0 876 22 50 35 -14 31 12 4.8 905 23 39 26 +43 55 12 3.2 Table 2. Brown Dwarf Candidates Name D RA Dec tint(total) pcs H M S D M S hours GL569B 10 *14 52 08 +16 18.3 0.4 GD165B 29 *14 22 12.0 +09 30 47 0.4 LHS2924 11 *14 26 36.1 +33 24 07.5 0.6 LHS1047B 5 00 12 53 -16 24.3 0.5 G29-38 14 23 26 15.0 +04 58 25.6 0.5 GL473B 4 12 30 51 +09 17.6 0.3 GL623B 7 *16 22 39 +48 28.4 0.4 PC0025+0447 - 00 25 07.3 +04 47 14 0.4 We will use microscanning for each object and each passband in the MD survey. Only CAM will be used for the survey, with the 3 arcsec PFOV, which provides a total array FOV of 1.5 arcmin. Except for the slight positional changes during the microscanning procedure, the array field will be centered on each M dwarf. CAM will be used for nearly all of the observations of the BD candidates. In all cases, the 1.5 arcsec pixel FOV will be used. For the one object that will be observed with ISOPHOT, photometry with PHT-P and a spectrum with PHT-S will be obtained. These observations are summarized in Table 3, where t(each) is the integration time for each discrete filter or at each CVF step, and t(all) is the total integration time for all the filters or for all the CVF scans. For the survey of 43 nearby M dwarfs using CAM, we will use the microscanning AOT for the two CAM passbands LW2 and LW3. Only those ttwo bands will be used for the survey, with both being used on each object. The observing modes and integration times for the seven individual BD candidates are presented in Table 3. For the MD/BD survey, we will observe each object for 64 seconds in each passband. If we allow 180 s to slew to the object, 2 s to rotate the filter wheel to each of the two filter positions, and 6 s as overhead for the 2x2 microcan, we derive a spacecraft time of 324 s to observe each survey object. Note that we will integrate for 16 s at each of the four microscan positions. For an autumn launch, the total spacecraft time to observe the 42 available survey objects will be 3.8 hours, whereas, for a spring launch it will take 3.0 hours of spacecraft time to observe the 33 available survey objects. For the eight BD candidates, the total integration time is the summation of the values of t(all) in Table 3, which is 3.5 hours. The space craft times for the individual candidates will be 4.9 h (Autumn) and 2.5 h (Spring).Note that we will use the ISO-supplied flat fields, which are expected to provide flat fielding accuracy at least as good as 1%. Table 3. Observing Modes for Brown-Dwarf Candidates Name Instrument Filter t(each) t(all) Comments sec hours GL569B CAM SW4,3 10 equal steps LW2,10,3 64 0.09 for each CVF CVF-SW = 30 steps CVF-LW1,LW2 32 0.27 ----------------------------------------------------------------- GD165B CAM SW4,3 LW2,10,7 256 0.36 ----------------------------------------------------------------- LHS2924 CAM SW4,3 6 equal steps LW2,10,3 64 0.09 for each CVF CVF-SW = 18 steps CVF-LW1,LW2 128 0.64 ----------------------------------------------------------------- LHS1047B PHOT P3.29,4.85,7.7 64 0.14 P11.3,16,20,25 124 0.05 S --- 0.35 ----------------------------------------------------------------- G29-38 CAM SW4,3 10 equal steps LW2,10,7,3 64 0.11 for each CVF CVF-LW1,LW2 64 0.36 = 20 steps ----------------------------------------------------------------- GL473B CAM CVF-SW 20 equal steps (Wolf 424) CVF-LW1,LW2 16 0.27 for each CVF = 60 steps ----------------------------------------------------------------- GL623B CAM SW4,3 10 equal steps LW2,10,3 64 0.09 for each CVF CVF-SW = 30 steps CVF-LW1,LW2 32 0.27 ----------------------------------------------------------------- PC0025+0447 CAM SW4,3 LW2 256 0.21 LW7 512 0.14 ----------------------------------------------------------------- REFERENCES Boss 1987, ApJ, 319, 149 Henry and McCarthy 1990, ApJ, 350, 334 Lunine 1986, in The Astrophysics of Brown Dwarfs, p.170 Probst 1986, in The Astrophysics of Brown Dwarfs, p.22 Skrutskie, Forrest, and Shure 1989, AJ, 98, 1409 Zuckerman and Becklin 1987, Nature, 330,138 <=== autumn_launch_targets ===> 1, "CAM01", 1.0, "N", "GL1002", 0.07028, -7.79167, 1950, 0., 0.,324,0 2, "CAM01", 1.0, "N", "GL15", 0.25861, 43.74000, 1950, 2.875, 0.404, 324,0 3, "CAM01", 1.0, "N", "GL54.1", 1.16639, -17.27333, 1950, 1.17, 0.62, 324,0 4, "CAM01", 1.0, "N", "GL83.1", 1.95778, 12.83500, 1950, 1.07, -1.79, 324,0 5, "CAM01", 1.0, "N", "GL166C", 4.21778, -7.73500, 1950, 0., 0., 324,0 6, "CAM01", 1.0, "N", "GL1111", 8.44806, 26.95333, 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