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The Complex Interstellar Na I Absorption toward h and χ Persei
Recent high spatial and spectral resolution investigations of thediffuse interstellar medium (ISM) have found significant evidence forsmall-scale variations in the interstellar gas on scales <=1 pc. Tobetter understand the nature of small-scale variations in the ISM, wehave used the Kitt Peak National Observatory (KPNO) WIYN Hydramultiobject spectrograph, which has a mapping advantage over thesingle-axis, single-scale limitations of studies using high propermotion stars and binary stars, to obtain moderate-resolution (~12 kms-1) interstellar Na I D absorption spectra of 172 starstoward the double open cluster h and χ Persei. All of the sightlines toward the 150 stars with spectra that reveal absorption from thePerseus spiral arm show different interstellar Na I D absorptionprofiles in the Perseus arm gas. Additionally, we have utilized the KPNOcoudé feed spectrograph to obtain high-resolution (~3 kms-1) interstellar Na I D absorption spectra of 24 of thebrighter stars toward h and χ Per. These spectra reveal an evengreater complexity in the interstellar Na I D absorption in the Perseusarm gas and show individual components changing in number, velocity, andstrength from sight line to sight line. If each of these individualvelocity components represents an isolated cloud, then it would appearthat the ISM of the Perseus arm gas consists of many small clouds.Although the absorption profiles vary even on the smallest scales probedby these high-resolution data (~30", ~0.35 pc), our analysis revealsthat some interstellar Na I D absorption components from sight line tosight line are related, implying that the ISM toward h and χ Per isprobably composed of sheets of gas in which we detect variations due todifferences in the local physical conditions of the gas.
| A 2dF survey of the Small Magellanic Cloud
We present a catalogue of new spectral types for hot, luminous stars inthe Small Magellanic Cloud (SMC). The catalogue contains 4161 objects,giving an order-of-magnitude increase in the number of SMC stars withpublished spectroscopic classifications. The targets are primarily B-and A-type stars (2862 and 853 objects respectively), with oneWolf-Rayet, 139 O-type and 306 FG stars, sampling the main sequence to~mid-B. The selection and classification criteria are described, andobjects of particular interest are discussed, including UV-selectedtargets from the Ultraviolet Imaging Telescope (UIT) experiment, Be andB[e] stars, `anomalous A supergiants' and composite-spectrum systems. Weexamine the incidence of Balmer-line emission, and the relationshipbetween Hγ equivalent width and absolute magnitude for BA stars.
| Search for Nanosecond Optical Pulses from Nearby Solar-Type Stars
With ``Earth 2000'' technology we could generate a directed laser pulsethat outshines the broadband visible light of the Sun by 4 orders ofmagnitude. This is a conservative lower bound for the technicalcapability of a communicating civilization; optical interstellarcommunication is thus technically plausible. We have built a pair ofsystems to detect nanosecond pulsed optical signals from a target listthat includes some 13,000 Sun-like stars, and we have made some 16,000observations totaling nearly 2400 hr during five years of operation. Abeam splitter-fed pair of hybrid avalanche photodetectors at the 1.5 mWyeth Telescope at the Harvard/Smithsonian Oak Ridge Observatory(Agassiz Station) triggers on a coincident pulse pair, initiatingmeasurement of pulse width and intensity at subnanosecond resolution. Anidentical system at the 0.9 m Cassegrain at Princeton's Fitz-RandolphObservatory performs synchronized observations with 0.1 μs eventtiming, permitting unambiguous identification of even a solitary pulse.Among the 11,600 artifact-free observations at Harvard, the distributionof 274 observed events shows no pattern of repetition, and is consistentwith a model with uniform event rate, independent of target. With onepossible exception (HIP 107395), no valid event has been seensimultaneously at the two observatories. We describe the search andcandidate events and set limits on the prevalence of civilizationstransmitting intense optical pulses.
| A Revised Calibration of the MV-W(O I 7774) Relationship using Hipparcos Data: Its Application to Cepheids and Evolved Stars
A new calibration of the MV-W(O I 7774) relationship hasbeen calculated using better reddening and distance estimates for asample of 27 calibrator stars of spectral types A to G, based onaccurate parallaxes and proper motions from the Hipparcos and Tychocatalogues. The present calibration predicts absolute magnitude withaccuracies of +/-0.38mag for a sample covering a large range ofMV, from -9.5 to +0.35 mag. The color term included in aprevious paper has been dropped since its inclusion does not lead to anysignificant improvement in the calibration. The variation of the O I7774 feature in the classical cepheid SS Sct has been studied. Wecalculated a phase-dependent correction to random phase OI featurestrengths in Cepheids, such that it predicts mean absolute magnitudesusing the above calibration. After applying such a correction, we couldincrease the list of calibrators to 58 by adding MV and O Itriplet strength data for 31 classical Cepheids. The standard error ofthe calibration using the composite sample was comparable to thatobtained from the primary 27 calibrators, showing that it is possible tocalculate mean Cepheid luminosities from random phase observations ofthe O I 7774 feature. We use our derived calibrations to estimateMV for a set of evolved objects to be able to locate theirpositions in the HR diagram.
| A Method for Simultaneous Determination of AV and R and Applications
A method for the simultaneous determination of the interstellarextinction (AV) and of the ratio of total to selectiveextinction (R), derived from the 1989 Cardelli, Clayton, & Mathisfitting of the interstellar extinction law, is presented and applied toa set of 1900 color excesses derived from observations of stars inUBVRIJHKL. The method is used to study the stability of AVand R within selected regions in Perseus, Scorpius, Monoceros, Orion,Sagittarius, Ophiuchus, Carina, and Serpens. Analysis shows that R isapproximately constant and peculiar to each sector, with mean valuesthat vary from 3.2 in Perseus to 5.6 in Ophiuchus. These results aresimilar to published values by Aiello et al., He et al., Vrba &Rydgren, O'Donnell, and Cardelli, Clayton, & Mathis.
| The Star Formation History and Mass Function of the Double Cluster h and χ Persei
The h and χ Per ``double cluster'' is examined using wide-field(0.98d×0.98d) CCD UBV imaging supplemented by optical spectra ofseveral hundred of the brightest stars. Restricting our analysis to nearthe cluster nuclei, we find identical reddenings [E(B-V)=0.56+/-0.01],distance moduli (11.85+/-0.05), and ages (12.8+/-1.0 Myr) for the twoclusters. In addition, we find an initial mass function slope for eachof the cluster nuclei that is quite normal for high-mass stars,Γ=-1.3+/-0.2, indistinguishable from a Salpeter value. We derivemasses of 3700 Msolar (h) and 2800 Msolar (χ)integrating the present-day mass function from 1 to 120Msolar. There is evidence of mild mass segregation within thecluster cores. Our data are consistent with the stars having formed at asingle epoch; claims to the contrary are very likely due to theinclusion of the substantial population of early-type stars located atsimilar distances in the Perseus spiral arm, in addition tocontamination by G and K giants at various distances. We discuss theuniqueness of the double cluster, citing other examples of suchstructures in the literature but concluding that the nearly identicalnature of the two cluster cores is unusual. We fail to settle thelong-standing controversy regarding whether or not the double cluster isthe core of the Per OB1 association and argue that this may beunanswerable with current techniques. We also emphasize the need forfurther work on the pre-main-sequence population of this nearby andhighly interesting region.
| H II Emission from a Complete Spectroscopic Survey of Be Stars in h and χ Persei
We describe data for emission-line B stars observed in a spectroscopicsurvey of h and χ Persei. The survey is complete to V=12.5 andcovers an area of ~1100 arcmin2 roughly centered on the twoclusters. We detect 32 Be stars; some have low Hα emissionstrength. Seven of these are new identifications; seven others areconfirmations of Be stars previously identified using photometry. Fiveof the observed Be stars show significant Hα profile variationsfrom epoch to epoch. We show that spectral indices yield physicalcharacteristics of the H II emission region. This automatic method isrobust and easily applied to large spectroscopic samples. We inferHα:Hβ flux ratios of 2-5 and observe a linear relationshipbetween Hα emission and J-K color for these stars. We include aHertzsprung-Russell diagram for the B-type stars in the clusters.
| UBVI and Hα Photometry of the h and χ Persei Cluster
UBVI and Hα photometry is presented for 17319 stars in vicinity ofthe young double cluster h and χ Persei. Our photometry extends overa 37'×1deg field centered on theassociation. We construct reddening contours within the imaged field. Wefind that the two clusters share a common distance modulus of11.75+/-0.05 and ages of logage(yr)=7.1+/-0.1. From the V-Hαcolor, a measure of the Hα emission strength, we conduct a surveyfor emission line objects within the association. We detect a sample of33 Be stars, eight of which are new detections. We present a scenario ofevolutionary enhancement of the Be phenomenon to account for the peak inBe fraction toward the top of the main sequence in the population of hand χ Persei and similar young clusters.
| Photometric study of the double cluster h & chi Persei
We present uvbybeta CCD photometry of the central region of the doublecluster h & chi Persei. We identify ~350 stars, of which 214 werenot included in Oosterhof's catalogue. Our magnitude limit V=16.5 allowsus to reach early F spectral type and obtain very accurate fits to theZAMS. We derive reddening values of E(b-y) = 0.44+/-0.02 for h Perseiand E(b-y) = 0.39+/-0.05 for chi Persei. From the ZAMS fitting, wederive distance moduli V0-MV = 11.66+/-0.20 andV0-MV = 11.56+/-0.20 for h and chi Perseirespectively. These values are perfectly compatible with both clustersbeing placed at the same distance and having identical reddenings. Theshift in the main-sequence turnoff and isochrone fitting, however, showthat there is a significant age difference between both clusters, withthe bulk of stars in h Persei being older than chi Persei. There is,however, a significant population of stars in h Persei which are youngerthan chi Persei. All this argues for at least three different epochs ofstar formation, corresponding approximately to log t = 7.0, 7.15 and 7.3Tables 2, 8 and 9 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/372/477. Based onobservations obtained with the Jacobus Kapteyn Telescope operated on theisland of La Palma by the Isaac Newton Group, in the SpanishObservatorio Roque de los Muchachos of the Instituto deAstrofísica de Canarias.
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| Understanding A-type supergiants. I. Ultraviolet and visible spectral atlas
This paper is the first of a series whose aim is to perform a systematicstudy of A-type supergiant atmospheres and winds. Here we present aspectral atlas of 41 A-supergiants observed by us in high and mediumresolution in the visible and ultraviolet. The atlas consists ofprofiles of the Hα , Hβ , Hγ , Hdelta , Hepsilon , CaII (H and K), Na I (D1 and D2), Mg II4481, Mg II [uv1] and FeII [uv1, uv2, uv3, uv62, uv63, uv161] lines for 41 stars with spectraltypes ranging from B9 to A9 and luminosity classes Ia, Iab and Ib, andprovides the basic data for a thoughtful study of these stars. Theoverall characteristics of the sample as well as the data reductionprocedures are described. We also present some examples of spectralvariability. Figures 1-3 are only available in electronic form at thehttp://www.edpsciences.com} of A-type supergiants\fnmsep\thanks{Based onobservations made with the INT and JKT telescopes operated on the islandof La Palma by the RGO in the Spanish Observatorio del Roque de LosMuchachos of the Instituto de Astrofisica de Canarias, with the 2.2~mtelescope at Calar Alto Observatory, Spain, with the Bernard Lyot 2~mtelescope at Pic Du Midi Observatory, France and observations collectedat the European Southern Observatory at La Silla, Chile.
| Understanding A-type supergiants. II. Atmospheric parameters and rotational velocities of Galactic A-type supergiants
We present the second paper of a series whose aim is to perform a globalstudy of Galactic A-supergiants. Very little work has been carried outto determine the stellar parameters of these stars. This is illustratedwith a brief review of some previous works. In this paper we analyze thedetermination of absolute magnitudes, spectral types and atmosphericparameters using the most recent Kurucz LTE blanketed model atmospheresand we discuss the applicability of the calibrations, such as theSchmidt-Kaler's (\cite{Sch-K}) calibration. Rotation is also animportant parameter in A-supergiants but their rotational velocities arepoorly known. We have calculated projected rotational velocities fromthe Fourier analysis of the observed Mg II (4481 Ä) line. Based onobservations made with the INT and JKT telescopes operated on the islandof La Palma by the RGO in the Spanish Observatorio del Roque de LosMuchachos of the Instituto de Astrofisica de Canarias, with the 2.2mtelescope at Calar Alto Observatory, Spain, with the Bernard Lyot 2mtelescope at Pic Du Midi Observatory, France and observations collectedat the European Southern Observatory at La Silla, Chile
| UBV beta Database for Case-Hamburg Northern and Southern Luminous Stars
A database of photoelectric UBV beta photometry for stars listed in theCase-Hamburg northern and southern Milky Way luminous stars surveys hasbeen compiled from the original research literature. Consisting of over16,000 observations of some 7300 stars from over 500 sources, thisdatabase constitutes the most complete compilation of such photometryavailable for intrinsically luminous stars around the Galactic plane.Over 5000 stars listed in the Case-Hamburg surveys still lackfundamental photometric data.
| Absolute Magnitudes and Colors of A-F Supergiants from Near-Infrared Features. II. The Galactic Sample
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2193S&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.
| Estimating absolute magnitudes and colors of A-F supergiants from near-infrared features. I - The Northern Hemisphere
In this paper we consider the calibration of the luminosity sensitive OI 7774 A feature in the A and F supergiants. We have obtained 2-3 Aresolution CCD spectra of this feature for nine A and F supergiants innorthern Galactic clusters. The new data, additional cluster members,and improvements in the various distance estimates have substantiallyimproved the calibration. We show that the intrinsic rms dispersionabout the resulting M(V)-W(lambda) relation for A and F supergiants iscomparable to that of the Cepheid period luminosity relation in thevisual. We have also found that an index measuring the strength of theinfrared calcium triplet provides an excellent indicator of intrinsiccolor among these stars. Together, these two relations suggest that Aand F supergiants could usefully be employed as standard candles out toat least 5 Mpc.
| Galactic OB associations in the northern Milky Way Galaxy. I - Longitudes 55 deg to 150 deg
The literature on all OB associations was reviewed, and their IRAS pointsource content was studied, between galactic longitude 55 and 150 deg.Only one third of the 24 associations listed by Ruprecht et al. (1981)have been the subject of individual studies designed to identify thebrightest stars. Distances to all of these were recomputed using themethod of cluster fitting of the B main sequence stars, which makes itpoossible to reexamine the absolute magnitude calibration of the Ostars, as well as for the red supergiant candidate stars. Also examinedwas the composite HR diagram for these associations. Associations withthe best defined main sequences, which also tend to contain very youngclusters, referred to here as OB clusters, have extremely few evolved Band A or red supergiants. Associations with poorly defined mainsequences and few OB clusters have many more evolved stars. They alsoshow an effect in the upper HR diagram referred to as a ledge byFitzpatrick and Garmany (1990) in similar data for the Large MagellanicCloud. It is suggested that the differences in the associations are notjust observational selection effects but represent real differences inage and formation history.
| Metallicity of the KHI Per cluster.
Not Available
| The catalogue of equivalent line widths in the spectra of A- and F-stars.
Not Available
| Geneva photometry of stars in the double cluster H and Chi Persei
Results are presented of a campaign of photometric observations of starsin the double cluster h and Chi Persei that spanned eight years. Thelong-time scale of the data has made it possible to discover that atleast half of the brighter stars in h and Chi Persei are variable stars.It appears that most of these variables are Be stars or related objects.Accurate color-magnitude diagrams for the brightest stars of the doublecluster show that the reddening is not as uniform as was assumed so far;that the observed parameters of many stars are very much affected by thehigh rotational velocities, and thus cannot be easily interpreted interms of physical quantities; and that the reported age and distancedifferences of both clusters are probably spurious. It is noted that thelarge intrinsic scatter of the colors and magnitudes of the h and ChiPersei stars casts doubt on the validity of photometric calibrationsthat rely heavily on observations of the double cluster.
| Miscellaneous spectroscopic notes
Results of slit-spectrograph observations are reported for approximately260 stars. The data presented range from recognition of many new Ap, Am,and other unusual stars to H-alpha observations of early-typesupergiants and Be stars. The material discussed was obtained over thepast 40 years at a number of U.S. observatories and at the DominionAstrophysical Observatory in Victoria, B.C.
| 2000 A UV imaging of a 6 deg diameter field around the H and Chi Persei double cluster
A stellar field centered close to the h and Chi per double cluster hasbeen observed at 2000 A by the stratospheric balloon-born telescope ofthe SCAP-2000 program. It is shown that the prevailing extinction lawproduces greater extinction at 1965 A than is predicted by the meanextinction law. The results suggest the presence of an H2 cloud in frontof h and Chi Per in the second absorbing layer and in the local arm. Agroup of hot stars centered at the same distance as the molecular cloudmay form an association of OB stars in the local arm.
| Interdependence of the 4430 A diffuse interstellar band, polarization, and ultraviolet extinction
Central intensities of the 4430-A diffuse interstellar band (DIB) areobtained from reticon spectra of 128 early-type stars, and stars in thePerseus OB1 association are found to have higher ratios of polarizationand weaker 4430-A intensities than do the stars in Cepheus OB3. Thecorrelation noted for OB1 between the A(4430) residuals and E(15-18) canbe explained if the 4430-A DIB arises in a thin grain mantle and the2200-A feature arises in the grain core. The absence of a 4430-A DIB inhigh-Galactic-latitude clouds would then be due to a lack of mantle. TheDIB ratio 5780/5797 A is found to resemble the behavior of the(4430-A)/E(B-V) ratio for seven stars from a range of Galacticlatitudes, confirming the existence of three previously identifiedfamilies of DIBs.
| Small Magellanic Cloud: H-gamma-line equivalent widths and luminosity classes of the brightest blue star members
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987A&AS...69..421A&db_key=AST
| Catalog of O-B stars observed with Tokyo Meridian Circle
A catalog of the O-B stars, selected from 'Blaauw-Parenago' list andRubin's catalog, has been compiled on the FK4 system by the observationsmade with Gautier 8-inch Meridian Circle at the Tokyo AstronomicalObservatory during the period, 1971 to 1979. It contains 1059 stars andwas compiled for the future establishment of high precision propermotions of O-B stars.
| Geneva intrinsic colours of the supergiants of spectral types A and F
The aim of this research note is to expose a photometric method todetermine the intrinsic values of the Geneva color index (B2-V1) for thesupergiants of spectral types A and F. The different stages which led tothis objective are presented, and the method is tested with a few starsbelonging to clusters for which color excesses were found in theliterature. A list of stars classified as supergiants which behavephotometrically as dwarfs is indicated.
| Near Infrared and Visual Photometry of H-Persei and Chi-Persei
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1984RMxAA...9...65T&db_key=AST
| Kinematic properties of supergiants in the Perseus spiral arm
Analysis of the space motions of supergiants in the Perseus arm regionindicates that the stellar peculiar-velocity field has a large-scalenonuniformity probably resulting both from the presence of sizablegroups of young stars and from systematic motions in the arm aspredicted by density-wave theory. Proper motions are tabulated for 78stars.
| Meridian observations made with the Carlsberg Automatic Meridian Circle at Brorfelde (Copenhagen University Observatory) 1981-1982
The 7-inch transit circle instrument with which the present position andmagnitude catalog for 1577 stars with visual magnitudes greater than11.0 was obtained had been equipped with a photoelectric moving slitmicrometer and a minicomputer to control the entire observationalprocess. Positions are reduced relative to the FK4 system for each nightover the whole meridian rather than the usual narrow zones. Thepositions of the FK4 stars used in the least squares solution are alsogiven in the catalog.
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Группы:
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Наблюдательные данные и астрометрия
| Созвездие: | Персей |
| Прямое восхождение: | 02h22m53.50s |
| Склонение: | +57°14'42.5" |
| Видимая звёздная величина: | 7.51 |
| Расстояние: | 2702.703 парсек |
| Собственное движение RA: | -0.2 |
| Собственное движение Dec: | -1.6 |
| B-T magnitude: | 8.23 |
| V-T magnitude: | 7.57 |
Каталоги и обозначения:
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