Contenidos
Imágenes
Subir su imagen
DSS Images Other Images
Artículos relacionados
The Orion Nebula in the Mid-Infrared
We present two wide-field (~5'×3&farcm;5),diffraction-limited (λ/D~=0.5" at 10 μm), broadband 10 and 20μm images of the Orion Nebula, plus six 7-13 μm narrowband(λ/Δλ~=1) images of the BN/KL complex taken at the3.8 m UKIRT telescope with the MPIA MAX camera. The wide-field images,centered on the Trapezium and BN/KL regions, are mosaics of35''×35'' frames obtained with standardchopping and nodding techniques and reconstructed using a newrestoration method developed for this project. They show the filamentarystructure of the dust emission from the walls of the H II region andreveal a new remarkable group of arclike structures ~1' to the south ofthe Trapezium. The morphology of the Ney-Allen Nebula, produced bywind-wind interaction in the vicinity of the Trapezium stars, suggests acomplex kinematical structure at the center of the cluster. We findindications that one of the most massive members of the cluster, theB0.5 V star θ1 Ori D, is surrounded by aphotoevaporated circumstellar disk. Among the four historic Trapezium OBstars, this is the only one without a binary companion, suggesting thatstellar multiplicity and the presence of massive circumstellar disks maybe mutually exclusive. In what concerns the BN/KL complex, we findevidence for extended optically thin silicate emission on top of thedeep 10 μm absorption feature. Assuming a simple two-component model,we map with ~=0.5" spatial resolution the foreground optical depth,color temperature, and mid-IR luminosity of the embedded sources. Weresolve a conspicuous point source at the location of the IRc2-A knot,approximately 0.5" north of the deeply embedded H II region ``I.'' Weanalyze the spectral profile of the 10 μm silicate absorption featureand find indication for grain crystallization in the harsh nebularenvironment. In the OMC-1 South region, we detect several point sourcesand discuss their association with the mass-loss phenomenology observedat optical and millimeter wavelengths. Finally, we list the position andphotometry of 177 point sources, the large majority of which aredetected for the first time in the mid-IR. Twenty-two of them lack acounterpart at shorter wavelengths and are therefore candidates fordeeply embedded protostars. The comparison of photometric data obtainedat two different epochs reveals that source variability at 10 μm ispresent up to a level of ~1 mag on a timescale of ~2 yr. With thepossible exception of a pair of OB stars, all point sources detected atshorter wavelengths display 10 μm emission well above thephotospheric level, which we attribute to disk circumstellar emission.The recent model of Robberto et al. provides the simplest explanationfor the observed mid-IR excess.
| Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i
This work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897
| Mapping the contours of the Local bubble: preliminary results
We present preliminary results from a long-term program of mapping theneutral absorption characteristics of the local interstellar medium,taking advantage of Hipparcos stellar distances. Equivalent widths ofthe NaI D-line doublet at 5890 Å are presented for thelines-of-sight towards some 143 new target stars lying within 300 pc ofthe Sun. Using these data which were obtained at the Observatoire deHaute Provence, together with previously published NaI absorptionmeasurements towards a further 313 nearby targets, we present absorptionmaps of the distribution of neutral gas in the local interstellar mediumas viewed from 3 different galactic projections. In particular, thesemaps reveal the Local Bubble region as a low neutral densityinterstellar cavity in the galactic plane with radii between 65-250 pcthat is surrounded by a (dense) neutral gas boundary (or ``wall''). Wehave compared our iso-column contours with the contours derived bySnowden et al. (\cite{snowden98}) using ROSAT soft X-ray emission data.Consistency in the global dimensions derived for both sets of contoursis found for the case of a million degree hot LB plasma of emissivity0.0023 cm(-6) pc with an electron density of 0.005 cm(-2) . We havedetected only one relatively dense accumulation of cold, neutral gaswithin 60 pc of the Sun that surrounds the star delta Cyg, and note thatthe nearest molecular cloud complex of MBM 12 probably resides at thevery edge of the Local Bubble at a distance of ~ 90 pc. Our observationsmay also explain the very different physical properties of the columnsof interstellar gas in the line-of-sight to the two hot stars epsilonCMa and beta CMa as being due to their locations with respect to theBubble contours. Finally, in the meridian plane the LB cavity is foundto be elongated perpendicularly to the Gould's Belt plane, possiblybeing ``squeezed'' by the expanding shells of the Sco-Cen andPerseus-Taurus OB associations. Tables 1 and 2 are also available inelectronic form at the CDS (Strasbourg) via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Spectral energy distributions and physical parameters of the atmospheres of main-sequence A stars with infrared excesses: Comparison with normal stars
For eight stars with infrared excesses greater than 0.5m in the IRASbands, we obtained the energy distribution over the range 3200-7600Angstroms and measured their infrared JHKLM magnitudes. Similarobservations were performed for 21 stars of various subclasses of thespectral type A with excesses no greater than 0.3m. Based on the energydistribution derived from the response curves of the photometric UBV andWBVR systems, we computed the synthetic B-V color indices, which are ingood agreement with the photometric observations. A comparison of thenormalized energy distribution in the spectra of A stars with infraredexcesses greater than 0.5m in the IRAS bands and the mean energydistribution for stars of the corresponding subclasses shows that themaximum difference does not exceed 10% both in the ultraviolet(3200-4000 Angstroms) and in the near infrared (up to 7600 Angstroms) Inall of the stars studied, we detected no excesses in the JHKLM bandsthat were greater than the accuracy of our measurements. Using themethod of infrared fluxes and comparing the observed energy distributionwith theoretical models of Kurucz, we determined the effectivetemperatures and angular diameters of the stars. For three stars, weestimated the parameters of their dust shells.
| The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS...99..135A&db_key=AST
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| Location and thickness of the nearest neutral gas cloud in the direction of Auriga-Perseus
High dispersion IUE spectra of stars in the general direction ofAuriga-Perseus show clear interstellar absorption lines whose strengthsare used to derive information about the spatial distribution of the gason the lines of sight. The distance to the nearest neutral cloud in thisdirection is about 50 pc; it has a depth of approximately 15 pc and adensity greater than 3/cu cm. Beyond the cloud the column densitieshardly increase, suggesting small gas densities out to about 200 pc.
| Third preliminary catalogue of stars observed with the photoelectric astrolabe of the Beijing Astronomical Observatory.
Not Available
| Location and thickness of the nearest gas cloud in the direction of Auriga-Perseus.
Not Available
| The Sirius supercluster
Photometric data on the chemical composition of 927 A stars in the UrsaMajor stream, called the Sirius supercluster, were used to estimate theage and place of formation of the objects. The stars studied are in thesolar neighborhood and have been observed to be co-moving in a velocityellipsoid with a (U, V) velocity of 10.3 km/sec and concentrated in aspatial volume less than 10 pc across. The Stromgren and Geneva systemphotometric data show that the supercluster is homogeneous in chemicalcontent, although the value of the forbidden Fe/H ratio could not beprecisely determined. The supercluster age is projected to be from260-620 Myr, with the origin having been in the Carina spiral arm of theGalaxy.
| Spectral classification from the ultraviolet line features of S2/68 spectra. III - Early A-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978A&AS...33...15C&db_key=AST
| Is star formation bimodal ? II. The nearest early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..187E&db_key=AST
| Absolute luminosity calibration of Stroemgren's 'late group'
A statistical parallax method based on the principle of maximumlikelihood is used to calibrate absolute luminosities for samples ofcooler stars constituting the 'late group' defined by Stromgren (1966).The samples examined include 415 stars of all luminosity classes and asubset comprising 86 main-sequence stars. Linear calibration relationsinvolving the Stromgren beta, (b-y), and bracketted c1 indices arederived which yield mean absolute magnitudes with an accuracy of 0.09magnitude for the overall sample and 0.13 magnitude for themain-sequence subsample. Several second-order relations are considered,and the results are compared with Crawford's (1975) calibrations as wellas with mean absolute magnitudes obtained from trigonometric parallaxes.The possible effect of interstellar absorption on the calibrationrelations is also investigated.
|
Enviar un nuevo artículo
Enlaces relacionados
- - No se han encontrado enlaces -
En viar un nuevo enlace
Miembro de los siguientes grupos:
|
Datos observacionales y astrométricos
| Constelación: | Cochero |
| Ascensión Recta: | 05h22m50.30s |
| Declinación: | +41°01'46.0" |
| Magnitud Aparente: | 5.54 |
| Distancia: | 91.996 parsecs |
| Movimiento Propio en Ascensión Recta: | -12.7 |
| Movimiento Propio en Declinación: | 4.4 |
| B-T magnitude: | 5.699 |
| V-T magnitude: | 5.559 |
Catálogos y designaciones:
|
