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APPLICATION for OBSERVING TIME : Multiplicity Of Time Allocation Committee for Application No. MPG time at the ESO 2.2m-telescope c/o MPI f¨urAstronomie Observing period October 2014 K¨onigstuhl17 Received D-69117 Heidelberg / Germany APPLICATION FOR OBSERVING TIME from MPIA MPG institute X other 1. Telescope: 2.2-m X 2.1 Applicant Rolf Chini Ruhr-Universit¨atBochum Name Institute Universit¨atsstraße150 44801 Bochum street ZIP code - city [email protected] ESO User Portal username e-mail 2.2 Collaborators Klaus Fuhrmann Ruhr-Universit¨atBochum name(s) institute(s) R´egisLachaume MPI f¨urAstronomie, Heidelberg name(s) institute(s) 2.3 Observers R´egisLachaume name name By specifying the names under item 2.3 it is obligatory to also send out these observers to La Silla, if required. Correspondence on the rating of this application will be sent to the applicant (P.I.) as quoted under 2.1 above. 3. Observing programme: Category: E Title : Multiplicity of stars as a function of mass Abstract : In the era of large Galactic surveys a major - yet mostly ignored - concern arises from the fact that up to one-third of the investigated samples will be subject to the polluting light of close and wide companion stars. To account for this circumstance, we aim at a thorough investigation of the stellar multiplicities as they are met around nearby stars in an unbiased, volume-complete sample and as a function of their primary masses. In analogy to our recent photometric search for distant companions to solar neighborhood stars, we do also expect to discover a number of stellar spectroscopic companions. We wish to finish our previous FEROS study in order to achieve a complete census of the spectroscopic binaries within 25 pc. 4. Instrument: WFI X FEROS GROND 5. Brightness range of objects to be observed: from 6 to 14 V-mag 6. Number of hours: applied for already awarded still needed 50 40 none no restriction grey dark 7. Optimum date range for the observations: ................................ 01.01.15 { 31.12.15 Usable range in local sideral time LST: ...................................... 00:00h { 24:00h 8a. Description of the observing programme Astrophysical context sphere is undoubtedly of general interest. By means of the FEROS spectrograph we intend complete the rel- The formation of stars has always been and continues evant observations of the final subsample of N∼ 100 to be one of the most diverse and complex topics in stars. modern astrophysics. Though, qualitatively, we known that stars are born in huge molecular gas clouds that can easily produce thousands of coeval objects, among Previous work the many unsolved questions is, what fraction of these Our previous work that includes all the nearby stars form in binaries or higher level systems, how much does in the Northern Hemisphere and down to declinations this depend on the environment, the fraction of early- δ ≥ −15o is summarized in Fuhrmann (2011). More re- type stars, their quasi-instantaneous feedback, or the cently, we started the southern observations of mostly complex dynamical processes involved. With respect to bright, F-type stars with the BESO ´echelle spectro- the latter point, much of the theoretical work in this graph at Cerro Armazones (Fuhrmann & Chini 2012). field considers the formation of stars in terms of bina- Thus, at the current stage of the project an 85 per ries, part of which may then be disrupted or expelled cent volume-completeness of the N∼ 500 star sample from a newly born cluster. However, the situation is is already achieved. very likely not that straightforward, since one must as- Not unexpectedly, it turned out that the inventory sume that more massive stars tend to create more com- of the stellar multiplicities at southern declinations is plex subunits, that is, hierarchical multiples consisting still fairly incomplete. Thus, in a very recent explo- of three, four, or even more components. Depending on rative survey, we found about a dozen new companion what stellar fraction is realized in terms of these mul- stars around FGK-type primaries within 25 pc from tiples, the general star formation process may proceed infrared photometry (Chini et al. 2014). We expect in a completely different manner. that part of these new companions will turn out to be In recent years, astrophysics has seen a growing in- spectroscopic binaries on their own (which we intend terest in large-scale stellar surveys (e.g. APOGEE, to find out with FEROS). RAVE, GAIA-ESO) on the formation and evolution In Fuhrmann & Chini (2012) we have already shown of the Milky Way. Among the basic science drivers is that there is a general decrease of the overall single- certainly the forthcoming launch of the GAIA satel- star fraction as a function of mass (cf. Fig. 1). But lite that aims at observations of about a billion stars even more, and as Fig. 2 demonstrates, there is also of our parent spiral. But on the other hand, there is a considerable lack of information on companion stars also the growing evidence that the merger-driven for- with the prospect that the importance of binary and mation scenario that one encounters in distant clusters higher-level systems may actually be much higher than of galaxies is eventually not realized in the Milky Way generally recognized. Galaxy. Among the N∼ 40 stars observed in 2014 February A major, yet mostly ignored, concern for the am- the majority has by now been analyzed and will be part bitious Galactic surveys however arises from the cir- of a forthcoming comprehensive study (Fuhrmann & cumstance that about 30 per cent of the investigated Chini 2014). For one of the companions, HD 43162 B, stars will turn out to be multiple (in the sense that we already found an asymmetry in the FEROS cross- more than one component contributes in the spectra). correlation function, suggestive for an SB2 system, and Even more, and given the considerable distances, wide in line with Janson et al. (2012), who recently resolved companions may not be resolvable, meaning that in this star as an M3.5 V + M5 V pair. addition to the numerous SB2 stars, a non-negligible fraction will turn out to be SB3 and SB4 systems. To meet these objects, it is of considerable impor- Layout of observations tance to learn from unbiased samples of nearby stars (i) The objects are distributed over all sideral times. what number and kind of systems one must expect and Therefore the project can serve as a filler project when- (ii) how to deal with the non-single light sources. Evi- ever time is available. For the G- and K-type primary dently, there must be a general interest in these items, stars we aim at redundant observations, preferably sep- because otherwise the multiple stars will not contribute arated by a few days (or months). For the fainter com- to, but pollute, existing correlations that one intends panion stars, and depending on whether they are SB1 to find with the Galactic surveys. or SB2 systems, it would be reasonable to follow those with repeated observations. Immediate aim The Hipparcos astrometric observations have estab- Strategic importance for MPIA lished a volume-complete reference sample of about R´egisLachaume will be co-author on all future publi- half a thousand solar-type stars within 25 pc. A thor- cations in this project. ough account of the basic stellar parameters as well as the stellar multiplicities that are met in this local 2 8b. Figures and tables Figure 1: Multiplicities of solar neighborhood stars as a function of their primary masses. The percentages of single, binary and higher level systems are presented in steps of 0:10 M , but as a running mean of bin width 0:20 M , with the number of stars per bin as indicated in the top of the figure. Average projected rotational velocities < v sin i > are depicted with a light blue shading. Except for the highest mass bins { which are mostly subject to Poisson noise (denoted by error bars) and high rotational velocities { there is a steady decline of the single-star fraction as a function of mass. (from Fuhrmann & Chini 2012) Figure 2: Same as Fig. 1, but with companion candi- dates included. Provided these candidates can be con- firmed, there is the prospect that the single-star frac- tion already converges to zero at the M ' 1:70 M transition to the A-type stars. (from Fuhrmann & Chini 2012) 3 9. Objects to be observed (Objects to be observed with high priority should be marked in last column) magnitude in Designation α (2000) δ (2000) spectral range priority to be observed HD 145825 16h 14m 11s:9 −31◦ 390 4900 6.55 1 HD 148704 A 16h 31m 30s:0 −39◦ 000 4400 7.24 1 HD 149612 16h 39m 04s:1 −58◦ 150 2900 7.03 1 HD 154088 17h 04m 27s:8 −28◦ 340 5700 6.59 1 HD 156274 A 17h 19m 03s:8 −46◦ 380 1000 5.47 1 HD 156274 B 17h 19m 02s:9 −46◦ 380 1300 8.70 1 HD 156897 A 17h 21m 00s:3 −21◦ 060 4600 4.40 1 HD 156897 B 17h 21m 00s:3 −21◦ 060 4600 8.90 1 HD 165185 A 18h 06m 23s:7 −36◦ 010 1100 5.95 1 HD 165185 B 18h 06m 23s:7 −36◦ 010 2300 13.0 1 HD 167425 A 18h 19m 40s:1 −63◦ 530 1100 6.16 1 HD 167425 B 18h 19m 39s:9 −63◦ 530 0400 10.8 1 HD 181321 19h 21m 29s:7 −34◦ 590 0000 6.47 1 HD 189567 20h 05m 32s:7 −67◦ 190 1500 6.49 1 HD 190422 20h 07m 35s:0 −55◦ 000 5700 6.25 1 HD 194640 20h 27m 44s:2 −30◦ 520 0400 6.62 1 HD 196761 20h 40m 11s:7 −23◦ 460 2500 6.38 1 HD 197214 A 20h 43m 15s:9 −29◦ 250 2600 6.95 1 HD 197214 B 20h 43m 14s:6 −29◦ 250 2200 13.0 1 HD 199288 20h 57m 40s:0 −44◦ 070 4500 6.52 1 HD 199509 21h 09m 20s:7 −82◦ 010 3800 7.00 1 HD 200525 AB 21h 09m 22s:5 −73◦ 100 2300 5.67 1 HD 200525 C 21h 09m 23s:7 −73◦ 100 2700 13.5 1 HD 202628 21h 18m 27s:2 −43◦ 200 0400
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