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Techniques for profile binning and analysis of eigenvector composite spectra: Comparing H beta and MgII lambda 2800 as virial estimators

Titulo: 
Techniques for profile binning and analysis of eigenvector composite spectra: Comparing H beta and MgII lambda 2800 as virial estimators
Autores: 
Sulentic, JW; Marziani, P; del Olmo, A; Plauchu-Frayn, I
Resumen: 
We review the basic techniques for extracting information about quasar structure and kinematics from the broad emission lines in quasars. We consider which lines can most effectively serve as virial estimators of black hole mass. At low redshift the Balmer lines, particularly broad H beta, are the lines of choice. For redshifts greater than 0.7 - 0.8 one can follow H beta into the IR windows or find an H beta surrogate. We explain why UV CIV lambda 1549 is not a safe virial estimator and how MgII lambda 2800 serves as the best virial surrogate for H beta up to the highest redshift quasar known at z approximate to 7. We show how spectral binning in a parameter space context (4DE1) makes possible a more effective comparison of H beta and MgII. It also helps to derive more accurate mass estimates from appropriately binned spectra and, finally, to map the dispersion in M-BH and Eddington ratio across the quasar population. FWHM MgII is about 20% smaller than FWHM H beta in the majority of type 1 AGN requiring correction when comparing MBH estimates from these two lines. The 20% of sources showing narrowest FWHM H beta (< 4000 km s(-1)) and strongest FeII (R-Fe greater than or similar to 1.0) emission (we call them bin A3-4 sources) do not show this FWHM difference and a blueshift detected in MgII for these sources suggests that FWHM H beta is the safer virial estimator for these extreme Eddington emitters. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.
Autor principal: 
Sulentic, JW
Autor/es del IAA: 
Sulentic, Jack W.; del Olmo, Ascension; Plauchu-Frayn, Ilse
DOI: 
10.1016/j.asr.2013.09.039
Revista: 
ADVANCES IN SPACE RESEARCH
Fecha de publicación: 
2014/10/01
Volumen: 
54
Issue: 
7
Páginas: 
1406-1413
Tipo de documento: 
Article
Palabras clave: 
Line:formation; Line: profile; Quasars: emission lines; Quasars: general

PumpKin: A tool to find principal pathways in plasma chemical models

Titulo: 
PumpKin: A tool to find principal pathways in plasma chemical models
Autores: 
Markosyan, AH; Luque, A; Gordillo-Vazquez, FJ; Ebert, U
Resumen: 
PumpKin is a software package to find all principal pathways, i.e. the dominant reaction sequences, in chemical reaction systems. Although many tools are available to integrate numerically arbitrarily complex chemical reaction systems, few tools exist in order to analyze the results and interpret them in relatively simple terms. In particular, due to the large disparity in the lifetimes of the interacting components, it is often useful to group reactions into pathways that recycle the fastest species. This allows a researcher to focus on the slow chemical dynamics, eliminating the shortest timescales. Based on the algorithm described by Lehmann (2004), PumpKin automates the process of finding such pathways, allowing the user to analyze complex kinetics and to understand the consumption and production of a certain species of interest. We designed PumpKin with an emphasis on plasma chemical systems but it can also be applied to atmospheric modeling and to industrial applications such as plasma medicine and plasma-assisted combustion. (C) 2014 Elsevier B.V. All rights reserved.
Autor principal: 
Markosyan, AH
Autor/es del IAA: 
Luque, A.; Gordillo-Vazquez, F. J.
DOI: 
10.1016/j.cpc.2014.05.019
Revista: 
COMPUTER PHYSICS COMMUNICATIONS
Fecha de publicación: 
2014/10
Volumen: 
185
Issue: 
10
Páginas: 
2697-2702
Tipo de documento: 
Article
Palabras clave: 
PumpKin; Pathway reduction; Chemical pathway analysis; Plasma chemistry; Pathway reduction; Plasma combustion

THE ALBEDO-COLOR DIVERSITY OF TRANSNEPTUNIAN OBJECTS

Titulo: 
THE ALBEDO-COLOR DIVERSITY OF TRANSNEPTUNIAN OBJECTS
Autores: 
Lacerda, P; Fornasier, S; Lellouch, E; Kiss, C; Vilenius, E; Santos-Sanz, P; Rengel, M; Muller, T; Stansberry, J; Duffard, R; Delsanti, A; Guilbert-Lepoutre, A
Resumen: 
We analyze albedo data obtained using the Herschel Space Observatory that reveal the existence of two distinct types of surface among midsized trans-Neptunian objects. A color-albedo diagram shows two large clusters of objects, one redder and higher albedo and another darker and more neutrally colored. Crucially, all objects in our sample located in dynamically stable orbits within the classical Kuiper Belt region and beyond are confined to the bright red group, implying a compositional link. Those objects are believed to have formed further from the Sun than the dark neutral bodies. This color-albedo separation is evidence for a compositional discontinuity in the young solar system.
Autor principal: 
Lacerda, P
Autor/es del IAA: 
Santos-Sanz, Pablo; Duffard, Rene
DOI: 
10.1088/2041-8205/793/1/L2
Revista: 
ASTROPHYSICAL JOURNAL LETTERS
Fecha de publicación: 
2014/09/20
Volumen: 
793
Issue: 
1
Tipo de documento: 
Article
Palabras clave: 
Kuiper belt: general

Theoretical study of the hydrogen bonding and infrared spectroscopy in the cis-vacant polymorph of dioctahedral 2:1 phyllosilicates

Titulo: 
Theoretical study of the hydrogen bonding and infrared spectroscopy in the cis-vacant polymorph of dioctahedral 2:1 phyllosilicates
Autores: 
Escamilla-Roa, E; Hernandez-Laguna, A; Sainz-Diaz, CI
Resumen: 
The spatial geometry and local environment of hydroxyl groups of the cis-vacant (cv) crystal polymorph of dioctahedral 2:1 phyllosilicates are studied by computational methods, doing especial emphasis on the hydrogen bonds and electrostatic interactions of the hydroxyl groups with the neighbor atoms. Different types of phyllosilicates are explored: with only tetrahedral charge, with only octahedral charge, with simultaneous octahedral and tetrahedral substitution, and with different interlayer cation (IC). The effect of these interactions on the spectroscopic properties of these hydroxyl groups is also studied. All results are compared with the trans-vacant (tv) crystal forms of these minerals. Frequency differences between cv and tv polymorphs are smaller than those due to the local environments of these OH groups. This means that the changes in the interactions of the different local environments of each OH group are greater than the cv/tv differences.
Autor principal: 
Escamilla-Roa, E
Autor/es del IAA: 
Escamilla-Roa, Elizabeth
DOI: 
10.1007/s00894-014-2404-4
Revista: 
JOURNAL OF MOLECULAR MODELING
Fecha de publicación: 
2014/09
Volumen: 
20
Issue: 
9
Tipo de documento: 
Article
Palabras clave: 
Cis-vacant; Clays; DFT; Hydrogen bonding; Infrared spectroscopy; Phyllosilicate; Polymorph
Número de artículo: 
2404

CLASH: A CENSUS OF MAGNIFIED STAR-FORMING GALAXIES AT z similar to 6-8

Titulo: 
CLASH: A CENSUS OF MAGNIFIED STAR-FORMING GALAXIES AT z similar to 6-8
Autores: 
Bradley, LD; Zitrin, A; Coe, D; Bouwens, R; Postman, M; Balestra, I; Grillo, C; Monna, A; Rosati, P; Seitz, S; Host, O; Lemze, D; Moustakas, J; Moustakas, LA; Shu, X; Zheng, W; Broadhurst, T; Carrasco, M; Jouvel, S; Koekemoer, A; Medezinski, E; Meneghetti, M; Nonino, M; Smit, R; Umetsu, K; Bartelmann, M; Benitez, N; Donahue, M; Ford, H; Infante, L; Jimenez-Teja, Y; Kelson, D; Lahav, O; Maoz, D; Melchior, P; Merten, J; Molino, A
Resumen: 
We utilize 16 band Hubble Space Telescope (HST) observations of 18 lensing clusters obtained as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program to search for z similar to 6-8 galaxies. We report the discovery of 204, 45, and 13 Lyman-break galaxy candidates at z similar to 6, z similar to 7, and z similar to 8, respectively, identified from purely photometric redshift selections. This large sample, representing nearly an order of magnitude increase in the number of magnified star-forming galaxies at z similar to 6-8 presented to date, is unique in that we have observations in four WFC3/UVIS UV, seven ACS/WFC optical, and all five WFC3/IR broadband filters, which enable very accurate photometric redshift selections. We construct detailed lensing models for 17 of the 18 clusters to estimate object magnifications and to identify two new multiply lensed z greater than or similar to 6 candidates. The median magnifications over the 17 clusters are 4, 4, and 5 for the z similar to 6, z similar to 7, and z similar to 8 samples, respectively, over an average area of 4.5 arcmin(2) per cluster. We compare our observed number counts with expectations based on convolving 'blank' field UV luminosity functions through our cluster lens models and find rough agreement down to similar to 27 mag, where we begin to suffer significant incompleteness. In all three redshift bins, we find a higher number density at brighter observed magnitudes than the field predictions, empirically demonstrating for the first time the enhanced efficiency of lensing clusters over field surveys. Our number counts also are in general agreement with the lensed expectations from the cluster models, especially at z 6, where we have the best statistics.
Autor principal: 
Bradley, LD
Autor/es del IAA: 
Benitez, N.; Jimenez-Teja, Y.; Molino, A.
DOI: 
10.1088/0004-637X/792/1/76
Revista: 
ASTROPHYSICAL JOURNAL
Fecha de publicación: 
2014/09/01
Volumen: 
792
Issue: 
1
Tipo de documento: 
Article
Palabras clave: 
galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong

MAGIC search for VHE gamma-ray emission from AE Aquarii in a multiwavelength context

Titulo: 
MAGIC search for VHE gamma-ray emission from AE Aquarii in a multiwavelength context
Autores: 
Aleksie, J; Ansoldi, S; Antonelli, LA; Antoranz, P; Babie, A; Bangale, P; Barrio, JA; Gonzalez, JB; Bedriarek, W; Bernardini, E; Biasuzzi, B; Biland, A; Blanch, O; Bonnefoy, S; Bonnoli, G; Borracci, E; Bretz, T; Carmona, E; Carosi, A; Colin, P; Colombo, E; Contreras, JL; Cortina, J; Covino, S; Da Vela, P; Dazzio, F; De Angelis, A; De Caneva, G; De Lotto, B; Wilhelmi, ED; Mendez, CD; Doert, M; Presters, DD; Dorner, D; Doro, M; Einecke, S; Eisenacher, D; Elsaesser, D; Fonseca, MV; Font, L; Frantzen, K; Fruck, C; Galindo, D; Lopez, RJG; Garczarczyk, M; Terrats, DG; Gaug, M; Godinovie, N; Munoz, AG; Gozzini, SR; Hadasch, D; Hanabata, Y; Hayashida, M; Herrera, J; Hildebrand, D; Hose, J; Hrupec, D; Idec, W; Kadenius, V; Kellermann, H; Kodani, K; Konno, Y; Krause, J; Kubo, H; Kushida, J; La Barbera, A; Lelas, D; Lewandowska, N; Lindfors, E; Lombardi, S; Lopez, M; Lopez-Coto, R; Lopez-Oramas, A; Lorenz, E; Lozano, I; Makariev, M; Mallot, K; Maneva, G; Mankuzhiyil, N; Mannheim, K; Maraschi, L; Marcote, B; Mariotti, M; Martinez, M; Mazin, D; Menzel, U; Miranda, JM; Mirzoyan, R; Moralejo, A; Munar-Adrover, P; Nakajima, D; Niedzwiecki, A; Nilsson, K; Nishijima, K; Noda, K; Nowak, N; Orito, R; Overkemping, A; Paiano, S; Palatiello, M; Paneque, D; Paoletti, R; Paredes, JM; Paredes-Fortuny, X; Persic, M; Moroni, PGP; Prandinin, E; Preziuso, S; Puljak, I; Reinthal, R; Rhode, W; Ribo, M; Rico, J; Garcia, JR; Rugamer, S; Saggion, A; Saito, T; Saito, K; Satalecka, K; Scalzotto, V; Scapin, V; Schultz, C; Schweizer, T; Sillanpaa, A; Sitarek, J; Snidaric, I; Sobczynska, D; Spanier, E; Stamatescu, V; Stamerra, A; Steinbring, T; Storz, J; Strzys, M; Takalo, L; Takami, H; Tavecchio, E; Temnikov, P; Terzie, T; Tescaro, D; Teshima, M; Thaele, J; Tibolla, O; Torres, DF; Toyama, T; Treves, A; Uellenbeck, M; Vogler, P; Wagner, RM; Zanin, R; Bogosavljevie, M; Ioannou, Z; Mauche, CW; Palaiologou, EV; Perez-Torres, MA; Tuommen, T
Resumen: 
Context. It has been claimed that the nova-like cataclysmic variable AE Aquarii (AE Aqr) is a very-high-energy (VHE, E > 100 GeV) source both on observational and theoretical grounds. Aims. We search for VHE gamma-ray emission from AE Aqr during different states of the source at several wavelengths to confirm or rule out previous claims of detection of gamma-ray emission from this object. Methods. We report on observations of AE Aqr performed by MAGIC. The source was observed during 12 h as part of a multiwavelength campaign carried out between May and June 2012 covering the optical, X-ray, and gamma-ray ranges. Besides MAGIC, the other facilities involved were the KVA, Skinakas, and Vidojevica telescopes in the optical and Swift in X-rays. We calculated integral upper limits coincident with different states of the source in the optical. We computed upper limits to the pulsed emission limiting the signal region to 30% of the phaseogram and we also searched for pulsed emission at different frequencies applying the Rayleigh test. Results. AE Aqr was not detected at VHEs during the multiwavelength campaign. We establish integral upper limits at the 95% confidence level for the steady emission assuming the differential flux proportional to a power-law function d phi/dE proportional to E-r, with a Crab-like photon spectral index of Gamma = 2.6. The upper limit above 200 GeV is 6.4 x 10(-12) cm(-2) s(-1) and above 1 TeV is 7.4 x 10(-13) cm(-2) s(-1). We obtained an upper limit for the pulsed emission of 2.6 x 10(-12) cm(-2) s(-1) for energies above 200 GeV. Applying the Rayleigh test for pulsed emission at different frequencies we did not find any significant signal. Conclusions. Our results indicate that AE Aqr is not a VHE gamma-ray emitter at the level of emission previously claimed. We have established the most constraining upper limits for the VHE gamma-ray emission of AE Aqr.
Autor principal: 
Aleksie, J
Autor/es del IAA: 
Perez-Torres, M. A.
DOI: 
10.1051/0004-6361/201424072
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/08
Volumen: 
568
Tipo de documento: 
Article
Palabras clave: 
accretion, accretion disks; radiation mechanisms: non-thermal; novae, cataclysmic variables; gamma rays: stars
Número de artículo: 
A109

Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations

Titulo: 
Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations
Autores: 
Barrera-Ballesteros, JK; Falcon-Barroso, J; Garcia-Lorenzo, B; van de Ven, G; Aguerri, JAL; Mendez-Abreu, J; Spekkens, K; Lyubenova, M; Sanchez, SE; Husemann, B; Mast, D; Garcia-Benito, R; Iglesias-Paramo, J; del Olmo, A; Marquez, I; Masegosa, J; Kehrig, C; Marino, RA; Verdes-Montenegro, L; Ziegler, B; MeIntosh, DH; Bland-Hawthorn, J; Walcher, CJ
Resumen: 
We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterise the kinematic orientation of non interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast external processes, such as major mergers. affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both stellar and nebular components and that internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components (similar to 90% of the sample has differences smaller than 16 degrees). This relation also holds, generally in barred galaxies across the bar and galaxy disc scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disc. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies.
Autor principal: 
Barrera-Ballesteros, JK
Autor/es del IAA: 
Sanchez, S. E.; Mast, D.; Garcia-Benito, R.; Iglesias-Paramo, J.; del Olmo, A.; Marquez, I.; Masegosa, J.; Kehrig, C.; Verdes-Montenegro, L.
DOI: 
10.1051/0004-6361/201423488
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/08
Volumen: 
568
Tipo de documento: 
Article
Palabras clave: 
galaxies: kinematics and dynamics; galaxies: photometry; galaxies: structure; galaxies: evolution
Número de artículo: 
A70

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Titulo: 
Recent activity of the Be/X-ray binary system SAX J2103.5+4545
Autores: 
Camero, A; Zurita, C; Gutierrez-Soto, J; Arabaci, MO; Nespoli, E; Kiaeerad, F; Beklen, E; Garcia-Rojas, J; Caballero-Garcia, M
Resumen: 
Aims. We present a multi wavelength study of the Be/X-ray binary system SAX J2103.5+4545 with the goal of better characterizing the transient behaviour of this source. Methods. SAXJ2103.5+4545 was observed by Swift/XRT four times in 2007 from April 25 to May 5, and during quiescence in 2012 August 31. In addition, this source has been monitored from the ground-based astronomical observatories of El Teide (Tenerife. Spain), Roque de los Muchachos (La Palma, Spain), and Sierra Nevada (Granada, Spain) since 2011 August, and from the TOM-TAR National Observatory (Antalya, Turkey) since 2009 June. We performed spectral and photometric temporal analyses to investigate the different states exhibited by SAXJ2103.5+4545. Results. In X-rays, an absorbed power-law model provided the best fit for all the XRT spectra. An iron-line feature at similar to 6.42 key was present in all the observations except for that taken during quiescence in 2012. The photon indexes are consistent with previous studies of SAX J2103.5+4545 in high/low-luminosity states, Pulsations were found in all the XRT data from 2007 (2.839(2) mHz; MJD 54 222.02), but not during quiescence. The two optical outbursts in 2010 and 2012 lasted for about eight or nine months (as the one in 2007 probably did and the current one in 2014 might do) and were most probably caused by mass-ejection events from the Be star that eventually fed the circumstellar disc. All of these outbursts started about three months before the triggering of the X-ray activity and at about the same period before the maximum of the Ho line equivalent width (in emission) was reached at only similar to 8-5 angstrom. The global correlation between the BV variability and the X-ray intensity was also observed at longer wavelengths in the IR domain.
Autor principal: 
Camero, A
Autor/es del IAA: 
Gutierrez-Soto, J.
DOI: 
10.1051/0004-6361/201423452
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/08
Volumen: 
568
Tipo de documento: 
Article
Palabras clave: 
accretion, accretion disks; pulsars: individual: SAX J2103.5+4545; X-rays: binaries; stars: emission line, Be
Número de artículo: 
A115

A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu

Titulo: 
A trio of gamma-ray burst supernovae: GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu
Autores: 
Cano, Z; Postigo, AD; Pozanenko, A; Butler, N; Thone, CC; Guidorzi, C; Kruhler, T; Gorosabel, J; Jakobsson, P; Leloudas, G; Malesani, D; Hjorth, J; Melandri, A; Mundell, C; Wiersema, K; D'Avanzo, P; Schulze, S; Gomboc, A; Johansson, A; Zheng, W; Kann, DA; Knust, F; Varela, K; Akerlof, CW; Bloom, J; Burkhonov, V; Cooke, E; de Diego, JA; Dhungana, G; Farina, C; Ferrante, FV; Flewelling, HA; Fox, OD; Fynbo, J; Gehrels, N; Georgiev, L; Gonzalez, JJ; Greiner, J; Guver, T; Hatch, N; Jelinek, M; Kehoe, R; Klose, S; Klunko, E; Kopae, D; Kutyrev, A; Krugly, Y; Lee, WH; Levan, A; Linkov, V; Matkin, A; Minikulov, N; Molotov, I; Prochaska, JX; Rieher, MG; Roman-Zuniga, CG; Rumyantsev, V; Sanchez-Ramirez, R; Steele, I; Tanvir, NR; Volnova, A; Watson, AM; Xu, D; Yuan, F
Resumen: 
We present optical and near-infrared (NIR) photometry for three gamma-ray burst supernovae (GRB-SNe): GRB 120729A, GRB 130215A/SN 2013ez, and GRB 130831A/SN 2013fu. For GRB 130215A/SN 2013ez, we also present optical spectroscopy at t-t(0) = 16.1 d, which covers rest-frame 3000-6250 angstrom. Based on Fell lambda 5169 and Sill lambda 6355, our spectrum indicates an unusually low expansion velocity of similar to 4000-6350 km s(-1), the lowest ever measured for a GRB-SN. Additionally, we determined the brightness and shape of each accompanying SN relative to a template supernova (SN 1998bw), which were used to estimate the amount of nickel produced via nucleosynthesis during each explosion. We find that our derived nickel masses are typical of other GRB-SNe, and greater than those of SNe Ibc that are not associated with GRBs. For GRB 130831A/SN 2013fu, we used our well-sampled R-band light curve (LC) to estimate the amount of ejecta mass and the kinetic energy of the SN, finding that these too are similar to other GRB-SNe. For GRB 130215A, we took advantage of contemporaneous optical/NIR observations to construct an optical/NIR bolometric LC of the afterglow. We fit the bolometric LC with the millisecond magnetar model of Zhang & Meszros (2001, ApJ, 552, L35), which considers dipole radiation as a source of energy injection to the forward shock powering the optical/NIR afterglow. Using this model we derive an initial spin period of P = 12 ms and a magnetic field of B = 1.1 x 10(15) G, which are commensurate with those found for proposed magnetar central engines of other long-duration GRBs.
Autor principal: 
Cano, Z
Autor/es del IAA: 
de Ugarte Postigo, A.; Thoene, C. C.; Gorosabel, J.; Jelinek, M.
DOI: 
10.1051/0004-6361/201423920
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/08
Volumen: 
568
Tipo de documento: 
Article
Palabras clave: 
gamma-ray burst: general; gamma-ray burst: individual: SN 2013ez; supernovae: general; supernovae: individual: SN 2013fu

Searching for delta Scuti-type pulsation and characterising northern pre-main-sequence field stars

Titulo: 
Searching for delta Scuti-type pulsation and characterising northern pre-main-sequence field stars
Autores: 
Diaz-Fraile, D; Rodriguez, E; Amado, PJ
Resumen: 
Context. Pre-main-sequence (PMS) stars objects evolving from the birthline to the zero age main sequence (ZAMS). Given a mass range near the ZAMS, the temperatures and luminosities of PMS and main-sequence stars are very similar. Moreover, their evolutionary tracks intersect one another causing some ambiguity in the determination of their evolutionary status. In this context, the detection and study of pulsations in PMS stars is crucial for differentiating between both types of stars by obtaining information of their interiors via asteroseismic techniques. Aims. A photometric variability study of a sample of northern field stars, which previously classified as either PMS or Herbig Ae/Be objects, has been undertaken with the purpose of detecting delta Scuti-type pulsations. Determination of physical parameters for these stars has also been carried out to locate them on the Hertzsprung-Russell diagram and check the instability strip for this type of pulsators. Methods. Multichannel photomultiplier and CCD time series photometry in the uvby Stromgren and BVI Johnson bands were obtained during four consecutive years from 2007 to 2010. The light curves have been analysed. and a variability criterion has been established. Among the objects classified as variable stars, we have selected those which present periodicities above 4 d(-1), which was established as the lowest limit for delta Scuti-type pulsations in this investigation. Finally, these variable stars have been placed in a colour magnitude diagram using the physical parameters derived with the collected uvby beta Stromgren-Crawford photometry. Results. Five PMS delta Scuti- and three probable beta Cephei-type stars have been detected. Two additional PMS delta Scuti stars are also confirmed in this work. Moreover, three new delta Scuti- and two gamma Doradus-type stars have been detected among the main-sequence objects used as comparison or check stars.
Autor principal: 
Diaz-Fraile, D
Autor/es del IAA: 
Diaz-Fraile, D.; Rodriguez, E.; Amado, P. J.
DOI: 
10.1051/0004-6361/201423478
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/08
Volumen: 
568
Tipo de documento: 
Article
Palabras clave: 
asteroseismology; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; stars: variables: delta Scuti; stars: fundamental parameters; Hertzsprung-Russell and C-M diagrams
Número de artículo: 
A32

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