- ID:
- ivo://CDS.VizieR/J/PASP/118/636
- Title:
- Alpha Per High res. spectral atlas at 3810-8100{AA}
- Short Name:
- J/PASP/118/636
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a high resolution (R=90000) spectral atlas of the F5Ib star Alpha Per covering the 3810-8100{AA} region. The atlas, based on data obtained with the aid of the echelle spectrograph BOES fed by 1.8-m telescope at Bohyunsan observatory (Korea) is a result of co-addition of a few well-exposed spectra. A final signal-to-noise ratio is ~800 at ~6000{AA}. The atlas is compared with the synthetic spectrum computed using the code based on (Kurucz, 1995, ASP Conf. Ser. 81, 583) software and databases. The adopted model atmosphere parameters are Teff=6240+/-20K, logg=0.58+/-0.04, and Vturb=3.20+/-0.05km/s. We also derived the iron abundance of [Fe/H]=-0.28+/-0.06. The spectral lines of Alpha Per have been identified by matching the synthetic spectrum with the observed one. The atlas is presented in figures and available in digital form at http://www.boao.re.kr/BOES/atlas/hd20902.html along with synthetic spectrum and spectral line identification tables.
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- ID:
- ivo://nasa.heasarc/alfperxmm
- Title:
- Alpha Per Open Cluster XMM-Newton X-Ray Source Catalog
- Short Name:
- ALFPERXMM
- Date:
- 11 Apr 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains results from the analysis of an archival XMM-Newton observation of part of the Alpha Persei open cluster. The authors detected 102 X-ray sources in the energy band from 0.3 to 8.0 keV, of which 39 of them are associated with the cluster as evidenced by their appropriate magnitudes and colors from Two Micron All Sky Survey (2MASS) photometry. In the reference paper, the authors extend the X-ray luminosity distribution (XLD) of the Alpha Persei cluster for M dwarfs, to add to the XLD found for hotter dwarfs from spatially extensive surveys of the whole cluster by ROSAT. Some of the hotter stars are identified as a background, possible slightly older group of stars at a distance of approximately 500 pc. Alpha Per is a young open cluster, found to be 50 Myr old from its upper main sequence turnoff morphology (Meynet et al. 1993, A&AS, 98, 477). More recently, Stauffer et al. (1999, ApJ, 527, 219) have found an age of 90 Myr from the low mass lithium depletion boundary. In addition to being relatively nearby (170 pc; Randich et al. 1996, A&A, 305, 785), the Alpha Per cluster is also lightly reddened (E(B - V ) = 0.09 mag; Meynet et al. 1993), making the data interpretation relatively robust. A fraction of the Alpha Per cluster was observed by XMM-Newton as part of the Mission Scientist Guaranteed Time (Pallavicini et al., 2004, MmSAI, 75, 434). A 60-ks observation was obtained on 2000 September 5 using the EPIC MOS and PN cameras on board XMM-Newton with a pointing centered at RA: 3<sup>h</sup> 26<sup>m</sup> 16<sup>s</sup> and Dec: 48<sup>o</sup> 50<sup>m</sup> 29<sup>s</sup> (J2000.0). This table was created by the HEASARC in June 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/AJ/145/143">CDS Catalog J/AJ/145/143</a> files table1.dat and table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://CDS.VizieR/J/AJ/123/1570
- Title:
- alpha Persei and Praesepe Clusters
- Short Name:
- J/AJ/123/1570
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Two hundred forty-two members of the Praesepe and alpha Persei clusters have been surveyed with high angular resolution 2.2{mu}m speckle imaging on the 3m Infrared Telescope Facility, the 5m Hale, and the 10m Keck telescopes, along with direct imaging using the near-infrared camera (NICMOS) aboard the Hubble Space Telescope. The observed stars range in spectral type from B (~5M_{sun}_) to early M (~0.5M_{sun}_), with the majority of the targets more massive than ~0.8M_{sun}_. The one quadruple and 39 binary systems detected encompass separations from 0.053" to 7.28"; 28 of the systems are new detections, and there are nine candidate substellar companions.
- ID:
- ivo://CDS.VizieR/J/AJ/131/2967
- Title:
- {alpha} Persei open cluster members
- Short Name:
- J/AJ/131/2967
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A kinematical study of the nearby open cluster {alpha} Persei is presented based on the astrometric proper motions and positions in the Tycho-2 catalog (Cat. I/259) and Second USNO CCD Astrographic Catalog (UCAC2, Cat. I/289). Using the astrometric data and photometry from the Tycho-2 and ground-based catalogs, 139 probable members of the cluster are selected, 18 of them new.
- ID:
- ivo://CDS.VizieR/J/A+A/628/A66
- Title:
- alpha Persei, Pleiades and Praesepe clusters
- Short Name:
- J/A+A/628/A66
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Our scientific goal is to provide revised membership lists of the alpha Per, Pleiades, and Praesepe clusters exploiting the second data release of Gaia and produce five-dimensional maps ({alpha}, {delta}, {pi}, {mu}_{alpha}_cos{delta}, {mu}_{delta}_) of these clusters. We implemented the kinematic method combined with the statistical treatment of parallaxes and proper motions to identify astrometric member candidates of three of the most nearby and best studied open clusters in the sky. We cross-correlated the Gaia catalogue with large-scale public surveys to complement the astrometry of Gaia with multi-band photometry from the optical to the mid-infrared. We identified 517, 1248, and 721 bona fide astrometric member candidates inside the tidal radius of alpha Per, the Pleiades, and Praesepe, respectively. We cross-matched our final samples with catalogues from previous surveys to address the level of completeness. We update the main physical properties of the clusters, including mean distance and velocity, as well as core, half-mass, and tidal radii. We infer updated ages from the white dwarf members of the Pleiades and Praesepe. We derive the luminosity and mass functions of the three clusters and compare them to the field mass function. We compute the positions in space of all member candidates in the three regions to investigate their distribution in space. We provide updated distances and kinematics for the three clusters. We identify a list of members in the alpha Per, Pleiades, and Praesepe clusters from the most massive stars all the way down to the hydrogen-burning limit with a higher confidence and better astrometry than previous studies. We produce complete 5D maps of stellar and substellar bona fide members in these three regions. The photometric sequences derived in several colour-magnitude diagrams represent benchmark cluster sequences at ages from 90 to 600Myr. We note the presence of a stream around the Pleiades cluster extending up to 40 pc from the cluster centre.
- ID:
- ivo://CDS.VizieR/J/A+A/367/859
- Title:
- {alpha} Scl and HD 170973 abundances
- Short Name:
- J/A+A/367/859
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Fine analyses of the magnetic CP stars {alpha} Scl and HD 170973 are presented using ATLAS9 model atmospheres which have same bulk metallicity as the deduced abundances. The light elements are mostly solar except for silicon, and all the heavier elements except nickel in HD 170973, which is solar, are greatly overabundant. The iron peak elements are typically 10 times overabundant, Sr is of order of 1000 times solar, Y and Zr are of order of 100 times solar. The rare earths are 1000 or more times overabundant.
- ID:
- ivo://CDS.VizieR/J/A+A/590/A54
- Title:
- alpha Vir RV and EW variations
- Short Name:
- J/A+A/590/A54
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Alpha Virginis (Spica) is a B-type binary system whose proximity and brightness allow detailed investigations of the internal structure and evolution of stars undergoing time-variable tidal interactions. Previous studies have led to the conclusion that the internal structure of Spica's primary star may be more centrally condensed than predicted by theoretical models of single stars, raising the possibility that the interactions could lead to effects that are currently neglected in structure and evolution calculations. The key parameters in confirming this result are the values of the orbital eccentricity e, the apsidal period U, and the primary star's radius, R1. The aim of this paper is to analyze the impact that Spica's line profile variability has on the derivation of its orbital elements and to explore the use of the variability for constraining R1.
- ID:
- ivo://CDS.VizieR/J/A+A/643/A4
- Title:
- ALPINE-ALMA [CII] survey. IR luminosity
- Short Name:
- J/A+A/643/A4
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ~4.4-5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 {mu}m obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope ({beta}), stellar mass (M*), and infrared excess (IRX=L_IR_/L_UV_). Twenty-three galaxies are individually detected in the continuum at > 3.5{sigma} significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z~4.4-5.8. The individual detections and stacks show that the IRX-{beta} relation at z~5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z<4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX-{beta} relation as a function of redshift suggests an evolution of dust attenuation properties at z>4. Similarly, we find that our galaxies have lower IRX values, up to 1dex on average, at a fixed mass compared to previously studied IRX-M* relations at z<=4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z>=4 are characterised by (i) a steeper attenuation curve than at z<=4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (logM*/M_{sun}_>10) at z~5-6 already exhibit an obscured fraction of star formation of ~45%, indicating a rapid build-up of dust during the epoch of reionization.
- ID:
- ivo://CDS.VizieR/J/A+A/643/A2
- Title:
- ALPINE DR1 merged catalog
- Short Name:
- J/A+A/643/A2
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The ALPINE-ALMA large program targets the [CII] 158um line and the far-infrared continuum in 118 spectroscopically confirmed star-forming galaxies between z=4.4 and z=5.9. It represents the first large [CII] statistical sample built in this redshift range. We present details of the data processing and the construction of the catalogs. We detected 23 of our targets in the continuum. To derive accurate infrared luminosities and obscured star formation rates, we measured the conversion factor from the ALMA 158um rest-frame dust continuum luminosity to the total infrared luminosity (LIR) after constraining the dust spectral energy distribution by stacking a photometric sample similar to ALPINE in ancillary single-dish far-infrared data. We found that our continuum detections have a median LIR of 4.4x10^11^L_{sun}_. We also detected 57 additional continuum sources in our ALMA pointings. They are at lower redshift than the ALPINE targets, with a mean photometric redshift of 2.5+/-0.2. We measured the 850um number counts between 0.35 and 3.5mJy, improving the current interferometric constraints in this flux density range. We found a slope break in the number counts around 3mJy with a shallower slope below this value. More than 40% of the cosmic infrared background is emitted by sources brighter than 0.35mJy. Finally, we detected the [CII] line in 75 of our targets. Their median [CII] luminosity is 4.8x108L_{sun}_ and their median full width at half maximum is 252km/s. After measuring the mean obscured SFR in various [CII] luminosity bins by stacking ALPINE continuum data, we find a good agreement between our data and the local and predicted SFR-L[CII] relations of De Looze et al. (2014A&A...568A..62D) and Lagache et al. (2018A&A...609A.130L).
- ID:
- ivo://CDS.VizieR/J/A+A/437/1147
- Title:
- Amalthea and Thebe CCD astrometric obs.
- Short Name:
- J/A+A/437/1147
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper presents the results of observations of Jupiter's satellites Amalthea and Thebe made in 1995, 1996 and 2001 at the Laboratorio Nacional de Astrofisica (LNA), Brazil. The observations were made in visible light wavelengths with a 1.6m reflector telescope and the light of Jupiter was covered by a mask placed near the CCD surface. The already published positions for 1995, whose astrometric reduction used the Galilean satellites, are now reduced using the stars in the CCD fields like the new positions of 1996 and 2001. The 2001 data are much better than those obtained in 1995, and that those from 1996 show large residuals. Considering the 310 frames observed, the mean residual is about 0.01" and the standard deviation is about 0.15".
