Contenuti
Immagini
Carica la tua immagine
DSS Images Other Images
Articoli relazionati
C18O Observations of the Dense Cloud Cores and Star Formation in Ophiuchus
In order to reveal the distribution of the dense gas of >=104cm3, C18O (J=1-0) observations have been madetoward the molecular clouds in the Ophiuchus region of ~6.4deg2 with the two 4 m telescopes of Nagoya University. Fortydense cores have been identified, providing the first complete sample ofsuch dense cores in Ophiuchus. The C18O dense cores aredistributed not only in the active star-forming region, ρ Oph cloudcore, but also in the North region where star formation is less active.The typical core mass, MLTE, radius, R, and average numberdensity, n(H2), of the cores are 90 Msolar, 0.24pc, and 1.7x104 cm-3 in the ρ Oph region,respectively, and 14 Msolar, 0.19 pc, and 7.6x103cm-3 in the North region, respectively. Nine of the 40 coresare associated with young stellar objects, and most of theC18O cores are starless. An analysis of the physicalparameters of the C18O cores show that star-forming corestend to have larger N(H2) than the rest by a factor of ~3,although there is no significant trend in the other physical parametersbetween star forming and starless cores. We have compared the presentC18O data with the 13CO data (Nozawa et al.) andwith the associated YSOs, in order to understand better the condensingprocess from molecular gas with density of ~103cm-3 to protostars. It is found that 55% of the13CO cores are associated with C18O cores and thatthe C18O cores are typically less massive, smaller and denserby ~34%, ~32%, and a factor of ~3, respectively, than the13CO cores. It is also found that the C18O coreshave steeper density profiles than the 13CO cores; when wefit the density profile by a power law as ρ~r-β, thevalues of β for C18O and 13CO are estimatedas ~1.5 and 1.2, respectively. This suggests that the C18Ocores are gravitationally more relaxed than the 13CO cores.In order to investigate the energetics of the cores, the virial mass,MVIR, has been calculated for each core. It is found thatmost of the 13CO cores have MVIR larger thanMLTE. On the other hand, 22 of the 40 C18O coreshave MVIR smaller than MLTE, suggesting that theC18O cores are more deeply gravitationally bound than the13CO cores. Further, we have found a correlation between theratio MVIR/MLTE and star formation activity: (1)For 13CO cores, the fraction of the 13CO coresassociated with the C18O cores tends to increase withdecreasing MVIR/MLTE, and (2) for theC18O cores, the fraction of the C18O coresassociated with stars tends to increase with decreasing ofMVIR/MLTE. We interpret this to indicate that thegradual dissipation of the internal turbulence leads to formation ofdenser cores and subsequent star formation. Through the evolution fromthe 13CO cores to the C18O cores, they should losethe turbulence energy of ~1044 ergs. The supersonic gasmotion with the magnetic fields produces shocks, and the radiation fromthe small shocked region may significantly contribute to the cooling. Wesuggest that the cores have continuous collisions between turbulenteddies to produce the C-shocks. Also, the Alfvénic energy lossmay be viable as the dissipation mechanism.
| Far-Ultraviolet Stellar Photometry: Fields Centered on rho Ophiuchi and the Galactic Center
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..104..101S&db_key=AST
| A homogeneous catalog of new UBV and H-beta photometry of B- and A-type stars in and around the Scorpius-Centaurus OB association
B- and A-type stars in and near the Sco-Cen OB association areinvestigated with UBV and H-beta photometry to acquire data relevant tothe luminosity function of Sco-Cen. The measurements generally consistof two 10-s integrations of U, B, V, (W, N) filters, and theobservations are corrected iteratively for atmospheric extinction andinstrumental response. The data presented give the mean V magnitude,mean B-V, mean U-B, and the estimated uncertainties for these values.The catalog provides a homogeneous catalog of data for a large fieldwith stellar objects delineating membership to the association Sco-Cenand that affect the luminosity function of the aggregate.
| Extinction law survey based on UV ANS photometry
The paper presents an extensive survey of interstellar extinction curvesderived from the ANS photometric measurements of early type starsbelonging to our Galaxy. This survey is more extensive and deeper thanany other one, based on spectral data. The UV color excesses aredetermined with the aid of 'artificial standards', a new techniqueproposed by the authors which allows the special check of Sp/L match ofa target and the selected standard. The results indicate that extinctionlaw changes from place to place.
| Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
| Empirical temperature calibrations for early-type stars
Three temperature calibrations of suitable photometric quantities havebeen derived for O and B stars. A sample of 120 stars with reliableT(eff.) determinations has been used for establishing each calibration.The different calibrations have been critically discussed and compared.Temperature determinations for 1009 program stars have been obtainedwith an accuracy of the order of 10 percent.
| Physical parameters of stars in the Scorpio-Centaurus OB association
Walraven photometry is presented of established and probable members ofthe Scorpio-Centaurus OB association. For each star, effectivetemperature and surface gravity are derived using Kurucz (1979)atmosphere models. From the Straizys and Kuriliene (1981) tables,absolute magnitudes are calculated. Distance moduli and visualextinctions are determined for all stars. From a comparison of theHR-diagrams of the stars in each subgroup with theoretical isochrones,the ages of the three subgroups are derived. The distances to the threesubgroups are shown to be different; there is a general trend (alsowithin each subgroup) for the distances to be larger at higher galacticlongitudes. The visual extinction in the youngest subgroupUpper-Scorpius, is well correlated with the IRAS 100-micron map. Thedistance toward the Ophiuchus dark clouds is found to be 125 pc, basedon the photometric distances to the stars. Most of the early-type starsin Upper-Scorpius are located at the far side of the dark clouds.
| The velocity field of the outer Galaxy in the southern hemisphere. III - Determination of distances to O, B, and A type stars in the Walraven photometric system
The Walraven photometric system has been used to derive distances tostars of spectral types earlier than A7. The details of the observingprocedure are given, and the way the data were analyzed is described.The accuracy of the data is discussed, and the results are compared withthose of Gathier et al. (1986). The observational results for stars ineight well-studied star cluster are presented, compared with theliterature, and discussed.
| E(B-V) determination from an UV-visual two-colour diagram - O and B stars in the Catalogue of Stellar Ultraviolet Fluxes
For the O and B type stars in the Catalogue of Stellar UltravioletFluxes, an approach is presented which does not require a preciseknowledge of spectral type and luminosity class for deriving E(B-V)color excesses. The method is based on the use of an UV-visual two-colordiagram; galactic variations in the interstellar extinction law areanalyzed and fully taken into account. The results have been comparedwith those derived by using the differences between observed andintrinsic colors for stars with known spectral classification. The verygood agreement in a large number of cases (94 percent) demonstrates thatthe present approach permits the derivation of reliable color excessvalues for early-type stars even if only a rough spectral classificationis available.
| A catalog of ultraviolet interstellar extinction excesses for 1415 stars
Ultraviolet interstellar extinction excesses are presented for 1415stars with spectral types B7 and earlier. The excesses with respect to Vare derived from Astronomical Netherlands Satellite (ANS) 5-channel UVphotometry at central wavelengths of approximately 1550, 1800, 2500, and3300 A. A measure of the excess extinction in the 2200-A extinction bumpis also given. The data are valuable for investigating the systematicsof peculiar interstellar extinction and for studying the character of UVinterstellar extinction in the general direction of stars for which theextinction-curve shape is unknown.
| An ultraviolet extinction study of the rho Ophiuchi dark cloud
Five-band ultraviolet spectrophotometry has been carried out for 54stars in the upper Scorpius complex. Of these, 14 stars in the rhoOphiuchi dark cloud and 13 in the surrounding area are found to be freeof spectral peculiarities and contamination by scattered light fromnearby bright stars. The dark cloud stars give extinction curves whichare significantly lower than the average extinction curves derived byother investigators and also those observed for localized regions suchas the area around Cygnus X-1 and the Cepheus OB III cluster. Thisimplies that the dust in the upper Scorpius region, especially that inthe rho Ophiuchi dark cloud has larger average size than the normalinterstellar medium. R, the ratio of total-to-selective extinction, isfound to be 4.2. The effects of a lower extinction curve on thechemistry of a dark cloud is also briefly discussed.
| On the origin of intermediate-latitude OB stars
An attempt is made to trace the origin of early-type stars observed atappreciable distances from the galactic plane. Because uncertainties inthe proper motions make space motions and hence dynamical lifetimesrather inaccurate, a theory of oscillations normal to the plane has beenused to compute radial velocities for 138 intermediate-latitude OBstars. These theoretical values are then compared with the observedradial velocities, and it is found that the low-velocity stars wereprobably ejected from the plane some time after formation, while thehigh-velocity stars were ejected very soon after formation. Velocitiesof ejection perpendicular to the plane are computed and show a narrowdistribution with a mean absolute value of 7 km/s together with a spreadof velocities from about 40 to over 200 km/s. The data are in reasonableagreement with a 'sling' effect and 'runaway' origin for the stars inthe sample.
| Radial velocities of southern early-type stars at intermediate galactic latitudes.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975MNRAS.172..649K&db_key=AST
| H-beta photometry of southern early-type stars and galactic structure away from the plane
H-beta photoelectric photometry is reported for 165 early-type stars atintermediate and high galactic latitudes. The data are combined withearlier UBV and spectroscopic results to determine the stellar spacedistribution. Stars of type B2 and earlier, at distances of up to 1 kpcfrom the galactic plane, appear to follow spiral structure in the plane.The available material, particularly the derived color excesses, is usedto select a number of blue stars which may be subluminous.
| UBV photometry of southern early-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974MNRAS.168..451H&db_key=AST
| Some Characteristics of the B and A Stars in the Upper Scorpius Complex
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1967ApJ...147.1003G&db_key=AST
| A Study of the II Scorpii Asscoiation.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1961ApJ...133..843H&db_key=AST
|
Sottometti un nuovo articolo
Link relazionati
Sottometti un nuovo link
Membro dei seguenti gruppi:
|
Osservazione e dati astrometrici
| Costellazione: | Ofiuco |
| Ascensione retta: | 16h47m29.75s |
| Declinazione: | -22°10'26.0" |
| Magnitudine apparente: | 9.334 |
| Moto proprio RA: | 2.5 |
| Moto proprio Dec: | -4.9 |
| B-T magnitude: | 9.409 |
| V-T magnitude: | 9.341 |
Cataloghi e designazioni:
|
