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1. An in-depth analysis of the differentially expanding star cluster Stock 18 (Villafranca O-036) using Gaia DR3 and ground-based data.

Author

Maíz Apellániz, J., Youssef, A. R., El-Nawawy, M. S., Elsanhoury, W. H., Sota, A., Pantaleoni González, M., and Ahmed, A.

Subjects
*STELLAR luminosity function, *SUPERGIANT stars, *STELLAR populations, *STAR clusters, *OPEN clusters of stars
Abstract

Context. The Villafranca project is combining Gaia data with ground-based surveys to analyze Galactic stellar groups (clusters, associations, or parts thereof) with OB stars. Aims. We want to analyze the poorly studied cluster Stock 18 within the Villafranca project, as it is a very young stellar cluster with a symmetrical and compact H II region around it, Sh 2-170, so it is likely to provide insights into the structure and dynamics of such objects at an early stage of their evolution. Methods. We used Gaia astrometry, photometry, spectrophotometry, and variability data as well as ground-based spectroscopy and imaging to determine the characteristics of Stock 18. We used these data to analyze its core, massive star population, extinction, distance, membership, internal dynamics, density profile, IMF, stellar variability, and Galactic location. Results. Stock 18 is a very young (∼1.0 Ma) cluster located at a distance of 2.91 ± 0.10 kpc and is dominated by the GLS 13 370 system, whose primary (Aa) is an O9 V star. We propose that Stock 18 was in a very compact state (∼0.1 pc) about 1.0 Ma ago and that most massive stars were ejected at that time without significantly affecting the less massive stars as a result of multi-body dynamical interactions. Different age estimates also point toward an age close to 1.0 Ma, indicating that the dynamical interactions took place very shortly after massive star formation. Well-defined expanding stellar clusters have been observed before, but none are as young as this one. If we include all of the stars, the initial mass function is top heavy, but if we discard the ejected ones, it becomes nearly canonical. Therefore, this is another example (in addition to the previous one we found – the Bermuda cluster) of (a) a very young cluster with an already evolved present day mass function (b) that has significantly contributed to the future population of free-floating compact objects. If confirmed in more clusters, the number of such compact objects may be higher in the Milky Way than previously thought. Stock 18 has a variable extinction with an average value of R5495 higher than the canonical one of 3.1. We have discovered a new visual component (Ab) in the GLS 13 370 system. The cluster is above our Galactic mid-plane, likely as a result of the Galactic warp, and it has a distinct motion with respect to its surrounding old population, which is possibly an influence of the Perseus spiral arm. [ABSTRACT FROM AUTHOR]

Published
2024
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4. The young stellar population of NGC 4214 as observed with HST. I. Data and methods

Author

Úbeda, Leonardo, Maíz-Apellániz, J., and MacKenty, John

Subjects
Astrophysics
Abstract

We present the data and methods that we have used to perform a detailed UV-optical study of the nearby dwarf starburst galaxy NGC 4214 using multifilter HST/WFPC2+STIS photometry. We explain the process followed to obtain high-quality photometry and astrometry of the stellar and cluster populations of this galaxy. We describe the procedure used to transform magnitudes and colors into physical parameters using spectral energy distributions. The data show the existence of both young and old stellar populations that can be resolved at the distance of NGC 4214 (2.94 Mpc) and we perform a general description of those populations., Comment: 33 pages, 9 figures, and 8 tables

Published
2007
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5. The young stellar population of NGC 4214 as observed with HST. II. Results

Author

Úbeda, Leonardo, Maíz-Apellániz, J., and MacKenty, John

Subjects
Astrophysics
Abstract

We present the results of a detailed UV-optical study of the nearby dwarf starburst galaxy NGC 4214 using multifilter HST/WFPC2+STIS photometry. The stellar extinction is found to be quite patchy, with some areas having values of E(4405-5495)< 0.1 mag and others, associated with star forming regions, much more heavily obscured, a result which is consistent with previous studies of the nebular extinction. We determined the ratio of blue-to-red supergiants and found it to be consistent with theoretical models for the metallicity of the SMC. The stellar IMF of the field in the range 20-100 solar masses is found to be steeper than Salpeter. A number of massive clusters and associations with ages between a few and 200 million years are detected and their properties are discussed., Comment: 49 pages, 12 figures, 6 tables

Published
2007
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6. Radio evidence on the mass loss bi-stability jump

Author

Benaglia, P., Vink, J. S., Marti, J., Maiz-Apellaniz, J., Koribalski, B., and Johnston, S.

Subjects
Astrophysics
Abstract

We present the results of a first campaign of radio continuum observations toward supergiants with spectral types in the range O8 - B3. Three targets out of twelve were detected with the ATCA and the VLA. The measured fluxes and the upper limits yielded values of the stellar mass-loss rates dM/dt and the wind efficiencies. The comparison of predicted and derived values of dM/dt shows a good agreement., Comment: Proceeding of the Conference Mass loss from stars and the evolution of stellar clusters

Published
2006

7. A cross-calibration between Tycho-2 photometry and HST spectrophotometry

Author

Maíz-Apellániz, J.

Subjects
Astrophysics
Abstract

I show that Tycho-2 photometry and HST spectrophotometry are accurate and stable enough to obtain a precise cross-calibration by analyzing a well-calibrated sample of 256 stars observed with both Hipparcos and HST. Based on this analysis, I obtain the following photometric zero points in the Vega magnitude system for Tycho-2: 0.020+-0.001 (B_T-V_T), 0.078+-0.009 (B_T), and 0.058+-0.009 (V_T)., Comment: 11 pages, 4 figures, to appear in Publications of the Astronomical Society of the Pacific (June 2005 issue)

Published
2005
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8. Young Super Star Clusters in the Starburst of M82: The Catalogue

Author

Melo, V. P., Muñoz-Tuñón, C., Maíz-Apellániz, J., and Tenorio-Tagle, G.

Subjects
Astrophysics
Abstract

Recent results from Hubble Space Telescope (HST) have resolved starbursts as collections of compact young stellar clusters. Here we present a photometric catalogue of the young stellar clusters in the nuclear starburst of M82, observed with the HST WFPC2 in Halpha (F656N) and in four optical broad-band filters. We identify 197 young super stellar clusters. The compactness and high density of the sources led us to develop specific techniques to measure their sizes. Strong extinction lanes divide the starburst into five different zones and we provide a catalogue of young super star clusters for each of these. In the catalogue we include relative coordinates, radii, fluxes, luminosities, masses, equivalent widths, extinctions, and other parameters. Extinction values have been derived from the broad-band images. The radii range between 3 and 9 pc, with a mean value of 5.7 +/- 1.4pc, and a stellar mass between 10e4 and 10e6 Mo. The inferred masses and mean separation, comparable to the size of super star clusters, together with their high volume density, provides strong evidence for the key ingredients postulated by Tenorio et al. (2003) as required for the development of a supergalactic wind., Comment: 45 pages, 5 figures, 12 tables. Accepted for publication in ApJ. Added Erratum

Published
2004
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9. CHORIZOS: a CHi-square cOde for parameteRized modelIng and characteriZation of phOtometry and Spectrophotometry

Author

Maíz-Apellániz, J.

Subjects
Astrophysics
Abstract

We have developed a CHi-square cOde for parameteRized modelIng and characteriZation of phOtometry and Spectrophotometry (CHORIZOS). CHORIZOS can use up to two intrinsic free parameters (e.g. temperature and gravity for stars; type and redshift for galaxies; or age and metallicity for stellar clusters) and two extrinsic ones (amount and type of extinction). The code uses chi-square minimization to find all models compatible with the observed data in the model N-dimensional (N=1,2,3,4) parameter space. CHORIZOS can use either correlated or uncorrelated colors as input and is especially designed to identify possible parameter degeneracies and multiple solutions. The code is written in IDL and is available to the astronomical community. Here we present the techniques used, test the code, apply it to a few well-known astronomical problems, and suggest possible applications. As a first scientific result from CHORIZOS, we confirm from photometry the need for a revised temperature-spectral type scale for OB stars previously derived from spectroscopy., Comment: 32 pages, 13 figures. To appear in the September 2004 issue of PASP

Published
2004
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10. The Progenitor of the Type II-P SN 2004dj in NGC 2403

Author

Maíz-Apellániz, J., Bond, H. E., Siegel, M. H., Lipkin, Y., Maoz, D., Ofek, E. O., and Poznanski, D.

Subjects
Astrophysics
Abstract

The Type II-P supernova 2004dj in the nearby galaxy NGC 2403 occurred at a position coincident with object 96 in the list of luminous stars and clusters in this galaxy published by Sandage in 1984. The coincidence is established definitively through astrometric registration of our ground-based archival images of NGC 2403 with our recent images showing the SN. The archival images show that Sandage 96 is slightly resolved from the ground. Pre-outburst blue spectrograms obtained by Humphreys and Aaronson reveal that Sandage 96 has a composite spectrum, dominated in the blue region by A- and B-type stars, while infrared photometry shows that Sandage 96 also contains red supergiants. These results demonstrate that Sandage 96 is a young compact cluster. We have studied the stellar population of Sandage 96, using published photometric measurements combined with a chi-square-fitting code. We derive a cluster age of 13.6 Ma, a reddening of E(4405-5495)=0.172, and a total stellar mass of 24 000 M_Sun. For this cluster age, the SN progenitor had a main-sequence mass of 15 M_Sun. Post-outburst photometry of Sandage 96 may establish whether the progenitor was a red or blue supergiant., Comment: Accepted for publication in ApJL. Replaces previous version not revised by the referee.13 pages, 3 figures

Published
2004
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11. NGC 604, the Scaled OB Association (SOBA) Prototype. I: Spatial Distribution of the Different Gas Phases and Attenuation by Dust

Author

Maíz-Apellániz, J., Pérez, E., and Mas-Hesse, J. M.

Subjects
Astrophysics
Abstract

We have analyzed HST and ground-based data to characterize the different gas phases and their interaction with the MYC in NGC 604, a GHR in M33. The warm ionized gas is made out of two components: a high-excitation, high-surface brightness H II surface located at the faces of the molecular clouds directly exposed to the ionizing radiation of the central SOBA; and a low-excitation, low-surface brightness halo that extends to much larger distances from the ionizing stars. The cavities created by the winds and SN explosions are filled with X-ray-emitting coronal gas. The nebular lines emitted by the warm gas experience a variable attenuation as a consequence of the dust distribution, which is patchy in the plane of the sky and with clouds interspersed among emission-line sources in the same line of sight. The optical depth at H alpha as measured from the ratio of the thermal radio continuum to H alpha shows a very good correlation with the total CO (1-0) column, indicating that most of the dust resides in the cold molecular phase. The optical depth at H alpha as measured from the ratio of H alpha to H beta also correlates with the CO emission but not as strongly as in the previous case. We analyze the difference between those two measurements and we find that <=11% of the H II gas is hidden behind large-optical-depth molecular clouds. We detect two candidate compact H II regions embedded inside the molecular cloud; both are within short distance of WR/Of stars and one of them is located within 16 pc of a RSG. We estimate the age of the main stellar generation in NGC 604 to be approx. 3 Myr from the ionization structure of the H II region. The size of the main cavity is smaller than the one predicted by extrapolating from single-star wind-blown bubbles., Comment: 50 pages, 15 figures. To appear in the September issue of the Astronomical Journal. Some of the figures in this version have a very low resolution due to the absurd limitations (for 2004) imposed on file size by astro-ph. A full-resolution version of the figures is available at http://www.stsci.edu/~jmaiz

Published
2004
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12. A Galactic O-Star Catalog

Author

Maíz-Apellániz, J., Walborn, N. R., Galué, H. Á., and Wei, L. H.

Subjects
Astrophysics
Abstract

We have produced a catalog of 378 Galactic O stars with accurate spectral classifications which is complete for V<8 but includes many fainter stars. The catalog provides cross-identifications with other sources; coordinates (obtained in most cases from Tycho-2 data); astrometric distances for 24 of the nearest stars; optical (Tycho-2, Johnson, and Stromgren) and NIR photometry; group membership, runaway character, and multiplicity information; and a web-based version with links to online services., Comment: 76 pages, 13 tables, and 3 figures. Accepted for publication in Astrophysical Journal. Online version of the catalog available at http://www.stsci.edu/~jmaiz/GOSmain.html

Published
2003
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13. Kinematical analysis of the ionized gas in the nuclear region of NGC 4214

Author

Maiz-Apellaniz, J., Munoz-Tunon, C., Tenorio-Tagle, G., and Mas-Hesse, J. M.

Subjects
Astrophysics
Abstract

We present in this paper a detailed study of the kinematical properties of the ionized gas around the young massive star clusters in the nucleus of NGC 4214. The analysis is based on bidimensional spectroscopical data, allowing to derive the spatial variation of different properties (intensity, velocity and width / line splitting) of the emission lines H\alpha and [O III] \lambda 5007 along the nuclear region. We have found that the Giant H II region around the two most massive clusters in NGC 4214 (A and B) is resolved into two clearly separated regions. We have not detected superbubbles with the properties we would expect according to the evolutionary state of the stellar clusters, but just a partial ring feature around the most massive one and two expanding shells around cluster B. The first expanding shell seems to have experienced blowout, whereas the second one is still complete. A possible explanation to this phenomenon is that the most massive stars in a starburst spend a large fraction of their lives buried inside their original molecular clouds. Champagne flows might have formed at the borders of the regions, especially on the SE complex, explaining the existence of the diffuse ionized gas around the galaxy. As a consequence of these results we postulate that NGC 4214 is indeed a dwarf spiral galaxy, with a thin (around 200 pc) disk that inhibits the formation of large scale structures in the ISM. The mechanical input deposited by the star formation complexes, in a variety of physical processes that include the free expanding bubbles liberated after blowout and photoevaporation of the parent clouds, have succeeded in generating the structures now detected far from the disk, giving place to the large-scale structure which now enriches the optical appearance of the galaxy., Comment: 18 pages, 13 figures, accepted for publication in Astronomy & Astrophysics

Published
1998

14. X-Shooting ULLYSES: Massive stars at low metallicity. I. Project description

Author

Vink, Jorick S., primary, Mehner, A., additional, Crowther, P. A., additional, Fullerton, A., additional, Garcia, M., additional, Martins, F., additional, Morrell, N., additional, Oskinova, L. M., additional, St-Louis, N., additional, ud-Doula, A., additional, Sander, A. A. C., additional, Sana, H., additional, Bouret, J.-C., additional, Kubátová, B., additional, Marchant, P., additional, Martins, L. P., additional, Wofford, A., additional, van Loon, J. Th., additional, Grace Telford, O., additional, Götberg, Y., additional, Bowman, D. M., additional, Erba, C., additional, Kalari, V. M., additional, Abdul-Masih, M., additional, Alkousa, T., additional, Backs, F., additional, Barbosa, C. L., additional, Berlanas, S. R., additional, Bernini-Peron, M., additional, Bestenlehner, J. M., additional, Blomme, R., additional, Bodensteiner, J., additional, Brands, S. A., additional, Evans, C. J., additional, David-Uraz, A., additional, Driessen, F. A., additional, Dsilva, K., additional, Geen, S., additional, Gómez-González, V. M. A., additional, Grassitelli, L., additional, Hamann, W.-R., additional, Hawcroft, C., additional, Herrero, A., additional, Higgins, E. R., additional, John Hillier, D., additional, Ignace, R., additional, Istrate, A. G., additional, Kaper, L., additional, Kee, N. D., additional, Kehrig, C., additional, Keszthelyi, Z., additional, Klencki, J., additional, de Koter, A., additional, Kuiper, R., additional, Laplace, E., additional, Larkin, C. J. K., additional, Lefever, R. R., additional, Leitherer, C., additional, Lennon, D. J., additional, Mahy, L., additional, Maíz Apellániz, J., additional, Maravelias, G., additional, Marcolino, W., additional, McLeod, A. F., additional, de Mink, S. E., additional, Najarro, F., additional, Oey, M. S., additional, Parsons, T. N., additional, Pauli, D., additional, Pedersen, M. G., additional, Prinja, R. K., additional, Ramachandran, V., additional, Ramírez-Tannus, M. C., additional, Sabhahit, G. N., additional, Schootemeijer, A., additional, Reyero Serantes, S., additional, Shenar, T., additional, Stringfellow, G. S., additional, Sudnik, N., additional, Tramper, F., additional, and Wang, L., additional

Published
2023
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15. The IACOB project

Author

Britavskiy, N., primary, Simón-Díaz, S., additional, Holgado, G., additional, Burssens, S., additional, Maíz Apellániz, J., additional, Eldridge, J. J., additional, Nazé, Y., additional, Pantaleoni González, M., additional, and Herrero, A., additional

Published
2023
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16. Orbital and physical properties of the sigma Ori Aa, Ab, B triple system

Author

Simón Díaz, S., Caballero, J. A., Lorenzo, J., Maíz Apellániz, J., Schneider, F. R. N., Negueruela, I., Barbá, R. H., Dorda, R., Marco, A., Montes Gutiérrez, David, Pellerin, A., Sánchez Bermúdez, J., Sódor, A., Sota, A., Simón Díaz, S., Caballero, J. A., Lorenzo, J., Maíz Apellániz, J., Schneider, F. R. N., Negueruela, I., Barbá, R. H., Dorda, R., Marco, A., Montes Gutiérrez, David, Pellerin, A., Sánchez Bermúdez, J., Sódor, A., and Sota, A.

Abstract

© 2015. The American Astronomical Society. All rights reserved. This research made use of SIMBAD, operated at Centre de Données astronomiques de Strasbourg, France, and NASA's Astrophysics Data System. Financial support was provided by the Spanish Ministerio de Ciencia e Innovación and Ministerio de Economía y Competitividad under grants AYA2010-17631, AYA2010-15081, AYA2010-21697-C05-04, AYA2011-30147-C03-03, AYA2012-39364-C02-01/02, and Severo Ochoa SEV-2011-0187, and by the Canary Islands Government under grant PID2010119. R.H.B. acknowledges support from FONDECYT Regular project 1140076. J.S.-B. acknowledges support by the JAE-PreDoc program of the Spanish Consejo Superior de Investigaciones Científicas (CSIC). A.S. acknowledges support by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. We acknowledge F. Najarro, J. Puls, A. Herrero, J. Casares, and H. Blau for interesting discussions during the development of this paper and their useful comments on one of the latest drafts before submission. We thank G. Schaefer for providing us some information about the results from the analysis of the interferometric observations prior to publication. Lastly, we thank the anonymous referee for a very professional report that helped us to improve the first version of the manuscript. Based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias. Based on observations made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Based on observations obtained with the HERMES spectrograph, which is supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of K.U. Leuven, Belgium, the Fonds National de la Recherche, We provide a complete characterization of the astrophysical properties of the sigma Ori Aa, Ab, B hierarchical triple system and an improved set of orbital parameters for the highly eccentric sigma Ori Aa, Ab spectroscopic binary. We compiled a spectroscopic data set comprising 90 high-resolution spectra covering a total time span of 1963 days. We applied the Lehman-Filhes method for a detailed orbital analysis of the radial velocity curves and performed a combined quantitative spectroscopic analysis of the sigma Ori Aa, Ab, B system by means of the stellar atmosphere code FASTWIND. We used our own plus other available information on photometry and distance to the system for measuring the radii, luminosities, and spectroscopic masses of the three components. We also inferred evolutionary masses and stellar ages using the Bayesian code BONNSAI. The orbital analysis of the new radial velocity curves led to a very accurate orbital solution of the sigma Ori Aa, Ab pair. We provided indirect arguments indicating that sigma Ori B is a fast-rotating early B dwarf. The FASTWIND+BONNSAI analysis showed that the Aa, Ab pair contains the hottest and most massive components of the triple system while sigma Ori B is a bit cooler and less massive. The derived stellar ages of the inner pair are intriguingly younger than the one widely accepted for the sigma Orionis cluster, at 3 +/- 1 Ma. The outcome of this study will be of key importance for a precise determination of the distance to the s Orionis cluster, the interpretation of the strong X-ray emission detected for sigma Ori Aa, Ab, B, and the investigation of the formation and evolution of multiple massive stellar systems and substellar objects., Spanish Ministerio de Ciencia e Innovación, Ministerio de Economía y Competitividad, Severo Ochoa, Canary Islands Government, FONDECYT Regular project, JAE-PreDoc program of the Spanish Consejo Superior de Investigaciones Científicas (CSIC), Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences, Fund for Scientific Research of Flanders (FWO), Belgium, Research Council of K.U. Leuven, Belgium, Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium, Royal Observatory of Belgium, Observatoire de Genève, Switzerland, Thringer Landessternwarte Tautenburg, Germany, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

17. Fundamental parameters of two O9-type giant stars: the (former) spectral classification standard HD 93249 A and ALS 12502 A.

Author

Ansín, T, Gamen, R, Morrell, N I, Barbá, R H, Maíz Apellániz, J, Arias, J I, Simón-Díaz, S, and Holgado, G

Subjects
SUPERGIANT stars, STELLAR evolution, CLASSIFICATION, MULTIPLICITY (Mathematics)
Abstract

The evolution of massive stars is not completely understood. Several phenomena affect their birth, life, and death, multiplicity being one of them. In this context, the OWN and MONOS projects are systematically observing O- and WN-type stars whose multiplicity status is unknown. Their major goal considers the necessity of determining absolute parameters of massive stars. We have collected spectra of HD 93249 A and ALS 12502 A aiming at characterizing their binary nature. For both stars, we analysed high-resolution spectra and combined them with Transiting Exoplanet Survey Satellite (TESS) observations to be compared with binary models constructed by means of the phoebe code. We discovered that the radial velocity of HD 93249 A varies with a period of 2.97968 ± 0.00001 d and that the system presents ellipsoidal light variations. We disentangled the composite spectra and classified its components as O9 III and B1.5 III, respectively. Confirmed as a spectroscopic binary, HD 93249 A can no longer be used as spectral classification standard. ALS 12502 A turned out to be a detached eclipsing binary in the TESS and Gaia data. These results enable us to determine absolute parameters for each component in the system. [ABSTRACT FROM AUTHOR]

Published
2023
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18. Gaia-ESO Survey: Massive stars in the Carina Nebula. I. A new census of OB stars

Author

Berlanas, S. R., primary, Maíz Apellániz, J., additional, Herrero, A., additional, Mahy, L., additional, Blomme, R., additional, Negueruela, I., additional, Dorda, R., additional, Comerón, F., additional, Gosset, E., additional, Pantaleoni González, M., additional, Molina Lera, J. A., additional, Sota, A., additional, Furst, T., additional, Alfaro, E. J., additional, Bergemann, M., additional, Carraro, G., additional, Drew, J. E., additional, Morbidelli, L., additional, and Vink, J. S., additional

Published
2023
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19. The VLT-FLAMES Tarantula Survey

Author

Sana, H., primary, Ramírez-Agudelo, O. H., additional, Hénault-Brunet, V., additional, Mahy, L., additional, Almeida, L. A., additional, de Koter, A., additional, Bestenlehner, J. M., additional, Evans, C. J., additional, Langer, N., additional, Schneider, F. R. N., additional, Crowther, P. A., additional, de Mink, S. E., additional, Herrero, A., additional, Lennon, D. J., additional, Gieles, M., additional, Maíz Apellániz, J., additional, Renzo, M., additional, Sabbi, E., additional, van Loon, J. Th., additional, and Vink, J. S., additional

Published
2022
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20. Massive stars in Carina from GES, GOSSS & LiLiMaRlin: A new census of OB stars to obtain a reliable distribution of rotational velocities for the O-star population

Author

Berlanas, S. R., Maíz Apellániz, J., and Herrero, A.

Subjects
OB stars, Massive stars, Rotational velocities, Carina
Abstract

The Carina Nebula is one of the major and more massive star-forming complexes of our Galaxy. It represents a unique region to study Galactic massive stars since it contains a large number of O-type stars that can be analyzed. Benefiting from large Galactic spectroscopic surveys such as the Gaia-ESO Survey (GES) and the Galactic O-Star Spectroscopic Survey (GOSSS), and the Library of Libraries of Massive-Star High-Resolution spectra (LiLiMaRlin), a detailed and comprehensive spectroscopic characterization of its massive stellar content can be performed to inspect the main physical properties of cluster members and test evolutionary and stellar atmospheres models. However, to obtain reliable results, a high degree of completeness in the census of its early-type population is mandatory. In this work, we present the most complete census of OB stars ever done in Carina. We provide accurate spectroscopic classifications for all the sample and determine rotational velocities for its O-star population. Thanks to this new spectroscopic census we have been able to obtain a reliable distribution of rotational velocities and compare it to other studies of O-stars in other Galactic and extra-Galactic regions.

Published
2022
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21. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author

Gilmore, G., primary, Randich, S., additional, Worley, C. C., additional, Hourihane, A., additional, Gonneau, A., additional, Sacco, G. G., additional, Lewis, J. R., additional, Magrini, L., additional, François, P., additional, Jeffries, R. D., additional, Koposov, S. E., additional, Bragaglia, A., additional, Alfaro, E. J., additional, Allende Prieto, C., additional, Blomme, R., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Van Eck, S., additional, Zwitter, T., additional, Bensby, T., additional, Flaccomio, E., additional, Irwin, M. J., additional, Franciosini, E., additional, Morbidelli, L., additional, Damiani, F., additional, Bonito, R., additional, Friel, E. D., additional, Vink, J. S., additional, Prisinzano, L., additional, Abbas, U., additional, Hatzidimitriou, D., additional, Held, E. V., additional, Jordi, C., additional, Paunzen, E., additional, Spagna, A., additional, Jackson, R. J., additional, Maíz Apellániz, J., additional, Asplund, M., additional, Bonifacio, P., additional, Feltzing, S., additional, Binney, J., additional, Drew, J., additional, Ferguson, A. M. N., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H.-W., additional, Vallenari, A., additional, Bergemann, M., additional, Casey, A. R., additional, de Laverny, P., additional, Frasca, A., additional, Hill, V., additional, Lind, K., additional, Sbordone, L., additional, Sousa, S. G., additional, Adibekyan, V., additional, Caffau, E., additional, Daflon, S., additional, Feuillet, D. K., additional, Gebran, M., additional, Gonzalez Hernandez, J. I., additional, Guiglion, G., additional, Herrero, A., additional, Lobel, A., additional, Merle, T., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Ruchti, G., additional, Soubiran, C., additional, Tabernero, H. M., additional, Tautvaišienė, G., additional, Traven, G., additional, Valentini, M., additional, Van der Swaelmen, M., additional, Villanova, S., additional, Viscasillas Vázquez, C., additional, Bayo, A., additional, Biazzo, K., additional, Carraro, G., additional, Edvardsson, B., additional, Heiter, U., additional, Jofré, P., additional, Marconi, G., additional, Martayan, C., additional, Masseron, T., additional, Monaco, L., additional, Walton, N. A., additional, Zaggia, S., additional, Aguirre Børsen-Koch, V., additional, Alves, J., additional, Balaguer-Nunez, L., additional, Barklem, P. S., additional, Barrado, D., additional, Bellazzini, M., additional, Berlanas, S. R., additional, Binks, A. S., additional, Bressan, A., additional, Capuzzo-Dolcetta, R., additional, Casagrande, L., additional, Casamiquela, L., additional, Collins, R. S., additional, D'Orazi, V., additional, Dantas, M. L. L., additional, Debattista, V. P., additional, Delgado-Mena, E., additional, Di Marcantonio, P., additional, Drazdauskas, A., additional, Evans, N. W., additional, Famaey, B., additional, Franchini, M., additional, Frémat, Y., additional, Fu, X., additional, Geisler, D., additional, Gerhard, O., additional, González Solares, E. A., additional, Grebel, E. K., additional, Gutiérrez Albarrán, M. L., additional, Jiménez-Esteban, F., additional, Jönsson, H., additional, Khachaturyants, T., additional, Kordopatis, G., additional, Kos, J., additional, Lagarde, N., additional, Ludwig, H.-G., additional, Mahy, L., additional, Mapelli, M., additional, Marfil, E., additional, Martell, S. L., additional, Messina, S., additional, Miglio, A., additional, Minchev, I., additional, Moitinho, A., additional, Montalban, J., additional, Monteiro, M. J. P. F. G., additional, Morossi, C., additional, Mowlavi, N., additional, Mucciarelli, A., additional, Murphy, D. N. A., additional, Nardetto, N., additional, Ortolani, S., additional, Paletou, F., additional, Palouš, J., additional, Pickering, J. C., additional, Quirrenbach, A., additional, Re Fiorentin, P., additional, Read, J. I., additional, Romano, D., additional, Ryde, N., additional, Sanna, N., additional, Santos, W., additional, Seabroke, G. M., additional, Spina, L., additional, Steinmetz, M., additional, Stonkuté, E., additional, Sutorius, E., additional, Thévenin, F., additional, Tosi, M., additional, Tsantaki, M., additional, Wright, N., additional, Wyse, R. F. G., additional, Zoccali, M., additional, Zorec, J., additional, and Zucker, D. B., additional

Published
2022
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22. The Tarantula Massive Binary Monitoring

Author

Shenar, T., primary, Sana, H., additional, Mahy, L., additional, Maíz Apellániz, J., additional, Crowther, Paul A., additional, Gromadzki, M., additional, Herrero, A., additional, Langer, N., additional, Marchant, P., additional, Schneider, F. R. N., additional, Sen, K., additional, Soszyński, I., additional, and Toonen, S., additional

Published
2022
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23. An excess of massive stars in the local 30 Doradus starburst

Author

Schneider, F. R. N., Sana, H., Evans, C. J., Bestenlehner, J. M., Castro, N., Fossati, L., Gräfener, G., Langer, N., Ramírez-Agudelo, O. H., Sabín-Sanjulián, C., Simón-Díaz, S., Tramper, F., Crowther, P. A., de Koter, A., de Mink, S. E., Dufton, P. L., Garcia, M., Gieles, M., Hénault-Brunet, V., Herrero, A., Izzard, R. G., Kalari, V., Lennon, D. J., Maíz Apellániz, J., Markova, N., Najarro, F., Podsiadlowski, Ph., Puls, J., Taylor, W. D., van Loon, J. Th., Vink, J. S., and Norman, C.

Published
2018
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24. Vela X-1 in depth: a review article on outstanding object

Author

Martínez-Núñez, Silvia, Kretschmar, Peter, El Mellah, I., Fuerst, F., Grinberg, V., Sander, A. A. C, van den Eijnden, J., Degenaar, N., Maíz Apellániz, J., Jiménez Esteban, F., Ramos-Lerate, M, and Utrilla, E.

Subjects
X-rays: individuals: Vela X-1, X-rays: binaries, stars: winds, outflows, accretion, accretion disks, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

In this poster, we will summarise the review paper entitled: "Revisiting the archetypical wind accretor Vela X-1 in depth. Case study of a well-known X-ray binary and the limits of our knowledge." The paper, published in late 2021 in Astronomy and Astrophysics journal, triggered a discussion amongst the editors of Astronomy and Astrophysics leading to the creation of a new type of review article on uniquely interesting objects. In the paper we have: provided a thoughtful compilation of the knowledge of the Vela X-1 system and its modelling published over decades; added new information derived from public data or catalogues, including an updated distance and spectral classification based on the Gaia EDR3 release; and identified specific avenues of future research that could help to clarify open questions.

Published
2022
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25. Vela X-1 in depth: a review article on an outstanding object

Author

Martínez-Núñez, Silvia, Kretschmar, Peter, El Mellah, I., Fuerst, F., Grinberg, V., Sander, A. A. C, van den Eijnden, J., Degenaar, N., Maíz Apellániz, J., Jiménez Esteban, F., Ramos-Lerate, M, and Utrilla, E.

Subjects
X-rays: individuals: Vela X-1, X-rays: binaries, stars: winds, outflows, accretion, accretion disks, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

In this poster, we will summarise the review paper entitled: "Revisiting the archetypical wind accretor Vela X-1 in depth. Case study of a well-known X-ray binary and the limits of our knowledge." The paper, published in late 2021 in Astronomy and Astrophysics journal, triggered a discussion amongst the editors of Astronomy and Astrophysics leading to the creation of a new type of review article on uniquely interesting objects. In the paper we have: provided a thoughtful compilation of the knowledge of the Vela X-1 system and its modelling published over decades; added new information derived from public data or catalogues, including an updated distance and spectral classification based on the Gaia EDR3 release; and identified specific avenues of future research that could help to clarify open questions., SMN acknowledges funding by the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER, UE), co-funded by FEDER funds and by the Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765.

Published
2022
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27. Massive Young Clusters

Author

Maíz-Apellániz, J., Burton, W. B., editor, Alfaro, Emilio J., editor, Pérez, Enrique, editor, and Franco, José, editor

Published
2004
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30. The Gaia-ESO Survey: The analysis of the hot-star spectra

Author

Blomme, R., primary, Daflon, S., additional, Gebran, M., additional, Herrero, A., additional, Lobel, A., additional, Mahy, L., additional, Martins, F., additional, Morel, T., additional, Berlanas, S. R., additional, Blazère, A., additional, Frémat, Y., additional, Gosset, E., additional, Maíz Apellániz, J., additional, Santos, W., additional, Semaan, T., additional, Simón-Díaz, S., additional, Volpi, D., additional, Holgado, G., additional, Jiménez-Esteban, F., additional, Nieva, M. F., additional, Przybilla, N., additional, Gilmore, G., additional, Randich, S., additional, Negueruela, I., additional, Prusti, T., additional, Vallenari, A., additional, Alfaro, E. J., additional, Bensby, T., additional, Bragaglia, A., additional, Flaccomio, E., additional, Francois, P., additional, Korn, A. J., additional, Lanzafame, A., additional, Pancino, E., additional, Smiljanic, R., additional, Bergemann, M., additional, Carraro, G., additional, Franciosini, E., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Jofré, P., additional, Magrini, L., additional, Morbidelli, L., additional, Sacco, G. G., additional, Worley, C. C., additional, and Zaggia, S., additional

Published
2022
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31. The Alma catalogue of OB stars – II. A cross-match with Gaia DR2 and an updated map of the solar neighbourhood

Author

Pantaleoni González, M., Maíz Apellániz, J., Barbá, R. H., Cameron Reed, B., Pantaleoni González, M. [0000-0001-9933-1229], Maíz Apellániz, J. [0000-0003-0825-3443], Barbá, R. H. [0000-0003-1086-1579], and Agencia Estatal de Investigación (AEI)

Subjects
solar neighbourhood [Galaxy], Astronometry, massive [Star], Catalogues, structure [Galaxy]
Abstract

We cross-match the Alma catalogue of OB stars with Gaia DR2 astrometry and photometry as a first step towards producing a clean sample of massive stars in the solar neighbourhood with a high degree of completeness. We analyse the resulting colour–absolute magnitude diagram to divide our sample into categories and compare extinction estimates from two sources, finding problems with both of them. The distances obtained with three different priors are found to have few differences among them, indicating that Gaia DR2 distances are robust. An analysis of the 3D distribution of massive stars in the solar neighbourhood is presented. We show that a kinematically distinct structure we dub the Cepheus spur extends from the Orion–Cygnus spiral arm towards the Perseus arm and is located above the Galactic mid-plane, likely being related to the recently discovered Radcliffe wave. We propose that this corrugation pattern in the Galactic disc may be responsible for the recent enhanced star formation at its crests and troughs. We also discuss our plans to extend this work in the immediate future. We thank the referee for a constructive report that helped us to improve the paper. MPG and JMA acknowledge support from the Ministerio de Ciencia, Innovación y Universidades through grant PGC2018-095049-B-C22. RHB acknowledges support from DIDULS Project 18 143 and the ESAC Faculty Visitor Program. This work has made use of data from the European Space Agency (ESA) Gaia mission, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of the SIMBAD data base, Aladin Sky Atlas, and the VizieR catalogue access tool, operated and developed by the Centre de Données astronomiques (CDS), Strasbourg Observatory, France, as well as TOPCAT, an interactive graphical viewer and editor for tabular data, and ASTROPY, a community-developed core Python package for Astronomy. Peerreview

Published
2021

33. The Villafranca catalog of Galactic OB groups

Author

Maíz Apellániz, J., primary, Barbá, R. H., additional, Fernández Aranda, R., additional, Pantaleoni González, M., additional, Crespo Bellido, P., additional, Sota, A., additional, and Alfaro, E. J., additional

Published
2022
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38. Revisiting the archetypical wind accretor Vela X-1 in depth

Author

Kretschmar, P., primary, El Mellah, I., additional, Martínez-Núñez, S., additional, Fürst, F., additional, Grinberg, V., additional, Sander, A. A. C., additional, van den Eijnden, J., additional, Degenaar, N., additional, Maíz Apellániz, J., additional, Jiménez Esteban, F., additional, Ramos-Lerate, M., additional, and Utrilla, E., additional

Published
2021
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40. The Tarantula Massive Binary Monitoring

Author

Shenar, T., primary, Sana, H., additional, Marchant, P., additional, Pablo, B., additional, Richardson, N., additional, Moffat, A. F. J., additional, Van Reeth, T., additional, Barbá, R. H., additional, Bowman, D. M., additional, Broos, P., additional, Crowther, P. A., additional, Clark, J. S., additional, de Koter, A., additional, de Mink, S. E., additional, Dsilva, K., additional, Gräfener, G., additional, Howarth, I. D., additional, Langer, N., additional, Mahy, L., additional, Maíz Apellániz, J., additional, Pollock, A. M. T., additional, Schneider, F. R. N., additional, Townsley, L., additional, and Vink, J. S., additional

Published
2021
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41. Galactic extinction laws – II. Hidden in plain sight, a new interstellar absorption band at 7700 Å broader than any known DIB

Author

Maíz Apellániz, J., Barbá, R. H., Caballero, J. A., Bohlin, R. C., Fariña, C., and Agencia Estatal de Investigación (AEI)

Subjects
Extinction, lines and bands [ISM], data analysis [Methods], dust [ISM], clouds [ISM], spectroscopic [Techniques], early type [Stars]
Abstract

This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) We have detected a broad interstellar absorption band centred close to 7700 Å and with a full width at half-maximum (FWHM) of 176.6 ± 3.9 Å. This is the first such absorption band detected in the optical range and is significantly wider than the numerous diffuse interstellar bands (DIBs). It remained undiscovered until now because it is partially hidden behind the A telluric band produced by O2. The band was discovered using STIS@HST spectra and later detected in a large sample of stars of diverse type (OB stars, BA supergiants, red giants), using further STIS and ground-based spectroscopy. The EW of the band is measured and compared with our extinction and K I λλ7667.021, 7701.093 measurements for the same sample. The carrier is ubiquitous in the diffuse and translucent Galactic interstellar medium (ISM) but is depleted in the environment around OB stars. In particular, it appears to be absent or nearly so in sightlines rich in molecular carbon. This behaviour is similar to that of the σ-type DIBs, which originate in the low/intermediate-density UV-exposed ISM but are depleted in the high-density UV-shielded molecular clouds. We also present an update on our previous work on the relationship between E(4405–5495) and R5495 and incorporate our results into a general model of the ISM. We thank an anonymous referee for useful comments and the STScI and earthbound telescope staffs for their help in acquiring the data for this paper. JMA and CF acknowledge support from the Spanish Government Ministerio de Ciencia through grant no. PGC2018095 049-B-C22. RHB acknowledges support from DIDULS Project 18 143 and the ESAC Faculty Visitor Program. JAC acknowledges support from the Spanish Government Ministerio de Ciencia through grant no. AYA2016-79 425-C3-2-P. Peerreview

Published
2021

42. The high-energy emission from the massive colliding-wind binary HD 93129A near periastron

Author

Del Palacio, S., Federico García, Altamirano, D., Corcoran, M., Hamaguchi, K., Barbá, R. H., Bosch-Ramon, V., Becker, M., Maíz Apellániz, J., Munar Adrover, P., Paredes, J. M., Romero, G. E., Sana, H., Tavani, M., Ud-Doula, A., and Astronomy

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. We present the results from our observations with the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We estimate the fraction of the wind kinetic power that is converted into relativistic electron acceleration and the magnetic field in the wind-collision region. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.

Published
2021

43. A comprehensive empirical investigation of Galactic fast-rotating O-type stars.

Author

Britavskiy, N., Holgado, G., Simón-Díaz, S., Maíz Apellániz, J., Pantaleoni González, M., Nazé, Y., Burssens, S., and Eldridge, J. J.

Subjects
EARLY stars, STELLAR evolution, STELLAR rotation, SUPERGIANT stars, BINARY stars
Abstract

Rotation is one of the important parameters affecting the evolution and final fate of massive stars but the origin of fast rotators remains unclear (imprint of the star formation process, result of binary interactions). In this work, we aim at investigating the binary status, photometric variability, and runaway status of a statistically meaningful sample of Galactic fast-rotating O stars. We perform a comprehensive multi-epoch analysis of new high-quality spectroscopic observations gathered by the IACOB and OWN surveys. Notably, we find that the total percentage of spectroscopic binaries in the investigated sample range between 25 and 40%, in agreement with previous finding for the case of O-type stars with lower projected rotational velocities. On the contrary, the fraction of runaway stars among fast rotators (∼35–50%) is significantly higher than in the case of slow rotators (∼20–30%). By combining all these observational results we will evaluate each scenario about the origin of fast rotators. [ABSTRACT FROM AUTHOR]

Published
2024
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44. Hubble spectroscopy of LB-1: Comparison with B+black-hole and Be+stripped-star models

Author

Lennon, D. J., primary, Maíz Apellániz, J., additional, Irrgang, A., additional, Bohlin, R., additional, Deustua, S., additional, Dufton, P. L., additional, Simón-Díaz, S., additional, Herrero, A., additional, Casares, J., additional, Muñoz-Darias, T., additional, Smartt, S. J., additional, González Hernández, J. I., additional, and de Burgos, A., additional

Published
2021
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45. outer orbit of the high-mass stellar triple system Herschel 36 determined with the VLTI.

Author

Sanchez-Bermudez, J, Hummel, C A, Díaz-López, J, Alberdi, A, Schödel, R, Arias, J I, Barbá, R H, Bastida-Escamilla, E, Brandner, W, Maíz Apellániz, J, and Pott, J-U

Subjects
VERY large telescopes, ORBITS (Astronomy), SUPERGIANT stars, PARALLAX
Abstract

Multiplicity is a ubiquitous characteristic of massive stars. Multiple systems offer us a unique observational constraint on the formation of high-mass systems. Herschel 36 A is a massive triple system composed of a close binary (Ab1-Ab2) and an outer component (Aa). We measured the orbital motion of the outer component of Herschel 36 A using infrared interferometry with the AMBER and PIONIER instruments of ESO's Very Large Telescope Interferometer. Our immediate aims are to constrain the masses of all components of this system and to determine if the outer orbit is co-planar with the inner one. Reported spectroscopic data for all two components of this system and our interferometric data allow us to derive full orbital solutions for the outer orbit Aa-Ab and the inner orbit Ab1-Ab2. For the first time, we derive the absolute masses of m Aa = 22.3 ± 1.7, m Ab1  = 20.5 ± 1.5, and m Ab2  = 12.5 ± 0.9 M⊙. Despite not being able to resolve the close binary components, we infer the inclination of their orbit by imposing the same parallax as the outer orbit. Inclinations derived from the inner and outer orbits imply a modest difference of about 22° between the orbital planes. We discuss this result and the formation of Herschel 36 A in the context of Core Accretion and Competitive Accretion models, which make different predictions regarding the statistic of the relative orbital inclinations. [ABSTRACT FROM AUTHOR]

Published
2022
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