J/A+A/556/A26ivo://CDS.VizieR/J/A+A/556/A26doi:10.26093/cds/vizier.35560026CDSHabibi M.Stolte A.Brandner W.Hussmann B.Motohara K.2013-08-05T12:12:12Z2013-07-19T09:30:53ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fropen-star-clustersinfrared-photometrystellar-massesThe Galactic Center is the most active site of star formation in the Milky Way Galaxy, where particularly high-mass stars have formed very recently and are still forming today. However, since we are looking at the Galactic Center through the Galactic disk, knowledge of extinction is crucial to study this region. The Arches cluster is a young, massive starburst cluster near the Galactic Center. We observed the Arches cluster out to its tidal radius using Ks-band imaging obtained with NAOS/CONICA at the VLT combined with Subaro/Cisco J-band data to gain a full understanding of the cluster mass distribution. We show that the determination of the mass of the most massive star in the Arches cluster, which had been used in previous studies to establish an upper-mass limit for the star formation process in the Milky Way, strongly depends on the assumed slope of the extinction law. Assuming the two regimes of widely used infrared extinction laws, we show that the difference can reach up to 30% for individually derived stellar masses and {Delta}AKs~1 magnitude in acquired Ks-band extinction, while the present mass function slope changes by ~0.17dex. The present-day mass function slope derived assuming the Nishiyama et al. (2009) extinction law increases from a flat slope of {alpha}-Nishi=-1.50+/-0.35 in the core (r<0.2pc) to {alpha}-Nishi=-2.21+/-0.27 in the intermediate annulus (0.2<r<0.4pc), where the Salpeter slope is -2.3. The present-day mass function steepens to {alpha}-Nishi=-3.21+/-0.30 in the outer annulus (0.4<r<1.5pc), indicating that the outer cluster region is depleted of high mass stars. This picture is consistent with mass segregation due to the dynamical evolution of the cluster.2013A&A...556A..26Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/556/A26CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)J/ApJ/581/258 : Infrared photometry in the Arches Cluster (Figer+, 2002)J/MNRAS/371/38 : X-ray observations of the Galaxy center (Wang+, 2006)J/ApJ/670/1115 : IRS spectra at 38 positions in GC (Simpson+, 2007)J/A+A/501/563 : HKs photometry in the Arches cluster (Espinoza+, 2009)J/ApJ/718/810 : Astrometry & photometry in the Arches cluster (Stolte+, 2010)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/556/A26https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/556/A26http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/556/A26https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/556/A26https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/556/A26http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/556/A26GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/556/A26/table5 (Photometry, mass and extinction in Arches cluster)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/556/A26/table5?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/556/A26/table5?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/556/A26/table5?GETtext/xml+votable180.050000true266.458525-28.823227780.0055555555555555566/288307.952274030004205e-20 1.7798557115773645e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/556/A26?format=asciiInfrareddefaultJ/A+A/556/A26/table5Photometry, mass and extinction in Arches clusterrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeqSequential numbermeta.recordintoRARight ascension offset from the reference star, J2000 (1)arcsecpos.eq.ra;arith.difffloatoDEDeclination offset from the reference star, J2000 (1)arcsecpos.eq.dec;arith.difffloatAKs(RL)? Ks-band extinction applying the RL-EL (2)magphys.absorptionfloatnullableAKs(N)? Ks-band extinction applying the N-EL (2)magphys.absorptionfloatnullableMi(RL)? Initial mass applying the RL-EL (2) (3)solMassphys.massdoublenullableM(RL)? Present mass applying the RL-EL (2) (3)solMassphys.massfloatnullableMi(N)? Initial mass applying the N-EL (2) (3)solMassphys.massfloatnullableM(N)? Present mass applying the N-EL (2) (3)solMassphys.massfloatnullableJmag[0/23.1]? J-band brightnessmagphot.mag;em.IR.JfloatnullableHmag[10.9/23.6]? H-band brightnessmagphot.mag;em.IR.HfloatnullableKsmag[0/33.4]? Ks-band brightnessmagphot.mag;em.IR.KfloatnullableA(Ks)[0/0.442]? estimated Ks-band extinctionmagphys.absorptionfloatnullableF[1/5] Cluster field in which the source is locatedobs.fieldintMm[0/1] Cluster members (1), others (0)meta.noteint_RAPositions computed from offsets (right ascension part)degpos.eq.ra;meta.main_DEPositions computed from offsets (declination part)degpos.eq.dec;meta.main