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511 results on '"Saviane, I."'

103. Soft gamma-ray selected giant radio galaxies: an update.

Author

Bassani, L, Ursini, F, Malizia, A, Bruni, G, Panessa, F, Masetti, N, Saviane, I, Monaco, L, Venturi, T, Dallacasa, D, Bazzano, A, and Ubertini, P

Subjects
RADIO galaxies, ACTIVE galactic nuclei, ACTIVE galaxies
Abstract

We present an update on the sample of soft gamma-ray selected giant radio galaxies (GRGs) extracted from INTEGRAL/IBIS and Swift /BAT surveys; it includes eight new sources and one candidate object. In the new sample, all but one source display FR II radio morphologies; the only exception is B21144+35B, which is an FR I. The objects belong to both type 1 and type 2 active galactic nucleus (AGN) optical classes and have redshifts in the range 0.06–0.35, while the radio sizes span from 0.7 to 1 Mpc. In this study, we present for the first time two objects that were never discussed as GRGs before and propose a new candidate GRG. We confirm the correlation between the X-ray luminosity and the radio core luminosity found for other soft gamma-ray selected GRGs and expected for AGNs powered by efficient accretion. We also corroborate previous results that indicate that the luminosity of the radio lobes is relatively low compared with the nuclear X-ray emission. This supports the idea that the nucleus of these GRGs is now more powerful than in the past, consistent with a restarting activity scenario. [ABSTRACT FROM AUTHOR]

Published
2021
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104. The transiting multi-planet system HD 3167: a 5 M⊕ super-earth and a 9 M⊕ mini-neptune

Author

Gandolfi, D., Barragan, O., Hatzes, A., Fridlund, Malcolm, Fossati, L., Donati, P., Johnson, M. C., Nowak, G., Prieto-Arranz, J., Albrecht, S., Dai, F., Deeg, H. J., Endl, M., Grziwa, S., Hjorth, M., Korth, J., Nespral, D., Saario, J., Smith, A. M. S., Antoniciello, G., Alarcon, J., Bedell, M., Blay, P., Brems, S., Cabrera, J, Csizmadia, S, Cusano, F., Cochran, W.D., Eigmüller, P, Erikson, A, Gonzalez Hernandez, J, Guenther, E., Hirano, T., Mascareno, S., Narita, N., Palle, E., Parviainen, H, Pätzold, M., Persson, C. M., Rauer, H, Saviane, I., Schmidtobreick, L., Van Eylen, V., Winn, J. N., and Zakhozhay, O.

Subjects
HD 3167 c, ​stars: fundamental parameters — stars: individual: HD 3167 — planets and satellites: detection — planets and satellites: individual: HD 3167 b
Published
2017

107. Variable broad lines and outflow in the weak blazar PBC J2333.9−2343

Author

Hernández-García, L, primary, Vietri, G, additional, Panessa, F, additional, Piconcelli, E, additional, Chavushyan, V, additional, Jiménez-Andrade, E F, additional, Bassani, L, additional, Bazzano, A, additional, Cazzoli, S, additional, Malizia, A, additional, Masetti, N, additional, Monaco, L, additional, Pović, M, additional, Saviane, I, additional, and Ubertini, P, additional

Published
2018
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110. On the Chemical Abundances of Miras in Clusters: V1 in the Metal-rich Globular NGC 5927

Author

D’Orazi, V., primary, Magurno, D., additional, Bono, G., additional, Matsunaga, N., additional, Braga, V. F., additional, Elgueta, S. S., additional, Fukue, K., additional, Hamano, S., additional, Inno, L., additional, Kobayashi, N., additional, Kondo, S., additional, Monelli, M., additional, Nonino, M., additional, Przybilla, N., additional, Sameshima, H., additional, Saviane, I., additional, Taniguchi, D., additional, Thevenin, F., additional, Urbaneja-Perez, M., additional, Watase, A., additional, Arai, A., additional, Bergemann, M., additional, Buonanno, R., additional, Dall’Ora, M., additional, Da Silva, R., additional, Fabrizio, M., additional, Ferraro, I., additional, Fiorentino, G., additional, Francois, P., additional, Gilmozzi, R., additional, Iannicola, G., additional, Ikeda, Y., additional, Jian, M., additional, Kawakita, H., additional, Kudritzki, R. P., additional, Lemasle, B., additional, Marengo, M., additional, Marinoni, S., additional, Martínez-Vázquez, C. E., additional, Minniti, D., additional, Neeley, J., additional, Otsubo, S., additional, Prieto, J. L., additional, Proxauf, B., additional, Romaniello, M., additional, Sanna, N., additional, Sneden, C., additional, Takenaka, K., additional, Tsujimoto, T., additional, Valenti, E., additional, Yasui, C., additional, Yoshikawa, T., additional, and Zoccali, M., additional

Published
2018
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111. Vista milky way public survey

Author

Minniti, D, Lucas, P, Ahumada, A, Zoccali, M, Catelan, M, Morelli, L, Tappert, C, Pignata, G, Toledo, I, Ruiz, M, Carraro, G, Casassus, S, Bronfman, L, Barbá, R, Gamen, R, Gieren, W, Geisler, D, Pietrzynski, G, Mennickent, R, Kurtev, R, Borissova, J, Mirabel, F, Ivanov, V, Saviane, I, and Vanzi, L

Abstract

We propose a public IR variability survey, named "Vista Variables in the Vía Láctea" (V V V ), of the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. This would take 1920 hours, covering ̃ 109 point sources within an area of 520 sq deg, including 33 known globular clusters and ̃ 350 open clusters. The final products will be a deep IR atlas in 5 passbands and a catalogue of ̃ 106 variable point sources. These will produce a 3-D map of the surveyed region (unlike single-epoch surveys that only give 2-D maps) using well-understood primary distance indicators such as RR Lyrae stars. It will yield important information on the ages of the populations. The observations will be combined with data from MACHO, OGLE, EROS, VST, SPITZER, HST, CHANDRA, INTEGRAL, and ALMA for a complete understanding of the variable sources in the inner Milky Way. Several important implications for the history of the Milky Way, for globular cluster evolution, for the population census of the bulge and center, and for pulsation theory would follow from this survey.

Published
2016

112. Globular Clusters and the Milky Way Connected by Chemistry

Author

Dias, B., Saviane, I., Barbuy, B., Held, E. V., Gary Da Costa, Ortolani, S., Gullieuszik, M., ITA, AUS, BRA, and CHL

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

There are two ways to study galaxy formation and evolution: one is to observe a large number of galaxies at a variety of redshifts, the other is to observe in detail just a few nearby galaxies. The precision achievable by the latter method enables the galactic history, including the formation and early evolution, to be studied. Globular clusters provide targets for the second method. We show how the chemical content of Milky Way globular clusters can be used to place them on a timeline charting the history of our Galaxy. The results suggest that different α-elements trace different processes of Milky Way chemical evolution.

Published
2016

115. Type II Cepheids in the Milky Way disc

Author

Lemasle, B., Kovtyukh, V., Bono, G., François, P., Saviane, I., Yegorova, I., Genovali, K., Inno, L., Galazutdinov, G., Da Silva, R., Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Astronomical observatory of Odessa National University [Odessa], Odessa National I.I.Mechnikov University, Institut de Mécanique des Fluides et des Solides (IMFS), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015

116. Improving the Quality of FORS2 Reduced Spectra

Author

Sabine Moehler, Dabo, C. E. G., Boffin, H., Rupprecht, G., Saviane, I., and Freudling, W.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The FORS2 instrument is one of the most widely used and productive instruments on the Very Large Telescope. This article reports on a project to improve the quality of the reduced FORS2 spectra that can be produced with the software provided by ESO. The result of this effort is that spectra of significantly higher quality can now be produced with substantially lower effort by the science user of the data., 5 pages, appeared in Messenger 159 (March 2015)

Published
2015

117. FORS2/VLT survey of Milky Way globular clusters

Author

Dias, B., Barbuy, B., Saviane, I., Held, E., DaCosta, G.S., Ortolani, S., Vasquez, S., Gullieuszik, M., Katz, D., Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo (USP), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2014

124. Properties of the solar neighbor WISE J072003.20−084651.2

Author

Ivanov, V. D., primary, Vaisanen, P., additional, Kniazev, A. Y., additional, Beletsky, Y., additional, Mamajek, E. E., additional, Mužić, K., additional, Beamín, J. C., additional, Boffin, H. M. J., additional, Pourbaix, D., additional, Gandhi, P., additional, Gulbis, A., additional, Monaco, L., additional, Saviane, I., additional, Kurtev, R., additional, Mawet, D., additional, Borissova, J., additional, and Minniti, D., additional

Published
2015
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125. VISTA Variables in the Vía Láctea (VVV): Current Status and First Results

Author

Saito, R., Hempel, M., Alonso García, J., Toledo, I., Borissova, J., González, O., Beamin J, C., Minniti, D., Lucas, P., Emerson, J., Ahumada, A., Aigrain, S., Alonso M, V., Amôres, E., Angeloni, R., Arias, J., Bandyopadhyay, R., Barbá, R., Barbuy, B., Baume, G., Bedin, L., Bica, E., Bronfman, L., Giovanni Carraro, Catelan, M., Clariá, J., Contreras, C., Cross, N., Davis, C., Grijs, R., Dékány, I., Janet Drew J, D., Fariña, C., Feinstein, C., Fernández Lajús, E., Folkes, S., Gamen, R., Geisler, D., Gieren, W., Goldman, B., Gosling, A., Gunthardt, G., Gurovich, S., Hambly, N., Hanson, M., Hoare, M., Irwin, M., Ivanov, V., Jordán, A., Kerins, E., Kinemuchi, K., Kurtev, R., Longmore, A., López Corredoira, M., Maccarone, T., Martín, E., Masetti, N., Mennickent, R., Merlo, D., Messineo, M., Mirabel, F., Monaco, L., Moni Bidin, C., LORENZO MORELLI, Padilla, N., Palma, T., Parisi M, C., Parker, Q., Pavani, D., Pietrukowicz, P., Pietrzynski, G., Pignata, G., Rejkuba, M., Rojas, A., Roman Lopes, A., Ruiz M, T., Sale, S., Saviane, I., Schreiber, M., Schröder, A., Sharma, S., Smith, M., Sodré L, Jr, Soto, M., Stephens, A., Tamura, M., Tappert, C., Thompson, M., Valenti, E., Vanzi, L., Weidmann, W., and Zoccali, M.

Published
2010

129. New VI CCD photometry of NGC 1851

Author

Saviane, I., Piotto, G., Fagotto, F., Zaggia, S., Aparicio, A., CAPACCIOLI, MASSIMO, Saviane, I., Piotto, G., Fagotto, F., Zaggia, S., Capaccioli, Massimo, and Aparicio, A.

Published
1995

133. Dynamical Modeling of the Deep Impact Dust Ejecta Cloud

Author

Bonev, T., primary, Ageorges, N., additional, Bagnulo, S., additional, Barrera, L., additional, Böhnhardt, H., additional, Hainaut, O., additional, Jehin, E., additional, Käufl, H. U., additional, Kerber, F., additional, LoCurto, G., additional, Manfroid, J., additional, Marco, O., additional, Pantin, E., additional, Pompei, E., additional, Saviane, I., additional, Selman, F., additional, Sterken, C., additional, Rauer, H., additional, Tozzi, G. P., additional, and Weiler, M., additional

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140. The relative ages of LMC old clusters, and the case of NGC 1841

Author

Saviane, I., Rosenberg, A., Antonio Aparicio, and Piotto, G.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Using archival HST/WFPC2 imaging of 7 LMC globular clusters, and following the methods outlined in our previous study, we have reached the tightest constrain so far on their age dispersion, which cannot be greater than ~ 0.5 Gyr. We also confirm earlier results that their average age is comparable to that of the metal-poor Galactic globulars. Evidence is also provided that NGC 1841 is younger than the rest of LMC globulars., Comment: 2 pages, 1 figure, requires newpasp.sty. To appear in "New Horizons in Globular Cluster Astronomy", Giampaolo Piotto, George Meylan, George Djorgovski and Marco Riello, eds

Published
2002
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142. The Optical SN 2012bz Associated with the Long GRB 120422A

Author

Melandri, A., Pian, E., Ferrero, P., D'Elia, V., Walker, E. S., Ghirlanda, G., Covino, S., Amati, L., D'Avanzo, P., Mazzali, P. A., Della Valle, M., Guidorzi, C., Antonelli, L. A., Bernardini, M. G., Bersier, D., Bufano, F., Campana, S., Castro-Tirado, A. J., Chincarini, G., Deng, J., Filippenko, A. V., Fugazza, D., Ghisellini, G., Kouveliotou, C., Maeda, K., Marconi, G., Masetti, N., Nomoto, K., Palazzi, E., Patat, F., Piranomonte, S., Salvaterra, R., Saviane, I., Starling, R. L. C., Tagliaferri, G., Tanaka, M., Vergani, S. D., Melandri, A., Pian, E., Ferrero, P., D'Elia, V., Walker, E. S., Ghirlanda, G., Covino, S., Amati, L., D'Avanzo, P., Mazzali, P. A., Della Valle, M., Guidorzi, C., Antonelli, L. A., Bernardini, M. G., Bersier, D., Bufano, F., Campana, S., Castro-Tirado, A. J., Chincarini, G., Deng, J., Filippenko, A. V., Fugazza, D., Ghisellini, G., Kouveliotou, C., Maeda, K., Marconi, G., Masetti, N., Nomoto, K., Palazzi, E., Patat, F., Piranomonte, S., Salvaterra, R., Saviane, I., Starling, R. L. C., Tagliaferri, G., Tanaka, M., and Vergani, S. D.

Abstract

The association of Type Ic SNe with long-duration GRBs is well established. We endeavor, through accurate ground-based observational campaigns, to characterize these SNe at increasingly high redshifts. We obtained a series of optical photometric and spectroscopic observations of the Type Ic SN2012bz associated with the Swift long-duration GRB120422A (z=0.283) using the 3.6-m TNG and the 8.2-m VLT telescopes. The peak times of the light curves of SN2012bz in various optical filters differ, with the B-band and i'-band light curves reaching maximum at ~9 and ~23 rest-frame days, respectively. The bolometric light curve has been derived from individual bands photometric measurements, but no correction for the unknown contribution in the near-infrared (probably around 10-15%) has been applied. Therefore, the present light curve should be considered as a lower limit to the actual UV-optical-IR bolometric light curve. This pseudo-bolometric curve reaches its maximum (Mbol = -18.56 +/- 0.06) at 13 +/- 1 rest-frame days; it is similar in shape and luminosity to the bolometric light curves of the SNe associated with z<0.2 GRBs and more luminous than those of SNe associated with XRFs. A comparison with the model generated for the bolometric light curve of SN2003dh suggests that SN2012bz produced only about 15% less 56Ni than SN2003dh, about 0.35 Msol. Similarly the VLT spectra of SN2012bz, after correction for Galactic extinction and for the contribution of the host galaxy, suggest comparable explosion parameters with those observed in SN2003dh (EK~3.5 x 10^52 erg, Mej~7 Msol) and a similar progenitor mass (~25-40 Msol). GRB120422A is consistent with the Epeak-Eiso and the EX,iso-Egamma,iso-E_peak relations. GRB120422A/SN2012bz shows the GRB-SN connection at the highest redshift so far accurately monitored both photometrically and spectroscopically., Comment: 7 pages, 6 figures, 2 tables, accepted for publication in Astronomy & Astrophysics

Published
2012
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144. VVV DR1: The First Data Release of the Milky Way Bulge and Southern Plane from the Near-Infrared ESO Public Survey VISTA Variables in the Via Lactea

Author

Saito, R. K., Hempel, M., Minniti, D., Lucas, P. W., Rejkuba, M., Toledo, I., Gonzalez, O. A., Alonso-Garcia, J., Irwin, M. J., Gonzalez-Solares, E., Hodgkin, S. T., Lewis, J. R., Cross, N., Ivanov, V. D., Kerins, E., Emerson, J. P., Soto, M., Amores, E. B., Gurovich, S., Dekany, I., Angeloni, R., Beamin, J. C., Catelan, M., Padilla, N., Zoccali, M., Pietrukowicz, P., Bidin, C. Moni, Mauro, F., Geisler, D., Folkes, S. L., Sale, S. E., Borissova, J., Kurtev, R., Ahumada, A. V., Alonso, M. V., Adamson, A., Arias, J. I., Bandyopadhyay, R. M., Barba, R. H., Barbuy, B., Baume, G. L., Bedin, L. R., Bellini, A., Benjamin, R., Bica, E., Bonatto, C., Bronfman, L., Carraro, G., Chene, A. N., Claria, J. J., Clarke, J. R. A., Contreras, C., Corvillon, A., de Grijs, R., Dias, B., Drew, J. E., Farina, C., Feinstein, C., Fernandez-Lajus, E., Gamen, R. C., Gieren, W., Goldman, B., Gonzalez-Fernandez, C., Grand, R. J. J., Gunthardt, G., Hambly, N. C., Hanson, M. M., Helminiak, K. G., Hoare, M. G., Huckvale, L., Jordan, A., Kinemuchi, K., Longmore, A., Lopez-Corredoira, M., Maccarone, T., Majaess, D., Martin, E. L., Masetti, N., Mennickent, R. E., Mirabel, I. F., Monaco, L., Morelli, L., Motta, V., Palma, T., Parisi, M. C., Parker, Q., Penaloza, F., Pietrzynski, G., Pignata, G., Popescu, B., Read, M. A., Rojas, A., Roman-Lopes, A., Ruiz, M. T., Saviane, I., Schreiber, M. R., Schroder, A. C., Sharma, S., Smith, M. D., Sodre Jr., L., Stead, J., Stephens, A. W., Tamura, M., Tappert, C., Thompson, M. A., Valenti, E., Vanzi, L., Walton, N. A., Weidmann, W., Zijlstra, A., Saito, R. K., Hempel, M., Minniti, D., Lucas, P. W., Rejkuba, M., Toledo, I., Gonzalez, O. A., Alonso-Garcia, J., Irwin, M. J., Gonzalez-Solares, E., Hodgkin, S. T., Lewis, J. R., Cross, N., Ivanov, V. D., Kerins, E., Emerson, J. P., Soto, M., Amores, E. B., Gurovich, S., Dekany, I., Angeloni, R., Beamin, J. C., Catelan, M., Padilla, N., Zoccali, M., Pietrukowicz, P., Bidin, C. Moni, Mauro, F., Geisler, D., Folkes, S. L., Sale, S. E., Borissova, J., Kurtev, R., Ahumada, A. V., Alonso, M. V., Adamson, A., Arias, J. I., Bandyopadhyay, R. M., Barba, R. H., Barbuy, B., Baume, G. L., Bedin, L. R., Bellini, A., Benjamin, R., Bica, E., Bonatto, C., Bronfman, L., Carraro, G., Chene, A. N., Claria, J. J., Clarke, J. R. A., Contreras, C., Corvillon, A., de Grijs, R., Dias, B., Drew, J. E., Farina, C., Feinstein, C., Fernandez-Lajus, E., Gamen, R. C., Gieren, W., Goldman, B., Gonzalez-Fernandez, C., Grand, R. J. J., Gunthardt, G., Hambly, N. C., Hanson, M. M., Helminiak, K. G., Hoare, M. G., Huckvale, L., Jordan, A., Kinemuchi, K., Longmore, A., Lopez-Corredoira, M., Maccarone, T., Majaess, D., Martin, E. L., Masetti, N., Mennickent, R. E., Mirabel, I. F., Monaco, L., Morelli, L., Motta, V., Palma, T., Parisi, M. C., Parker, Q., Penaloza, F., Pietrzynski, G., Pignata, G., Popescu, B., Read, M. A., Rojas, A., Roman-Lopes, A., Ruiz, M. T., Saviane, I., Schreiber, M. R., Schroder, A. C., Sharma, S., Smith, M. D., Sodre Jr., L., Stead, J., Stephens, A. W., Tamura, M., Tappert, C., Thompson, M. A., Valenti, E., Vanzi, L., Walton, N. A., Weidmann, W., and Zijlstra, A.

Abstract

The ESO Public Survey VISTA Variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for ~5 years. In this paper we describe the progress of the survey observations in the first observing season, the observing strategy and quality of the data obtained. The observations are carried out on the 4-m VISTA telescope in the ZYJHKs filters. In addition to the multi-band imaging the variability monitoring campaign in the Ks filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHKs filters taken in the 2010 observing season. The typical image quality is ~0.9-1.0". The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHKs images in the disk area and 90% of the JHKs images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28x10^8 stellar sources in the bulge and 1.68x10^8 in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63x10^8 stellar sources. About 10% of these are double detections due to overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHKs bands extend typically ~4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for Ks=15-18 mag has rms ~35-175 mas., Comment: Accepted for publication in Astronomy and Astrophysics (Section 14: Catalogs and data)

Published
2011
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145. The VISIR@VLT Mid-IR view of 47Tuc: A further step in solving the puzzle of RGB mass loss

Author

Momany, Y., Saviane, I., Smette, A., Bayo, A., Girardi, L., Marconi, G., Milone, A. P., Bressan, A., Momany, Y., Saviane, I., Smette, A., Bayo, A., Girardi, L., Marconi, G., Milone, A. P., and Bressan, A.

Abstract

There is an ongoing debate regarding the onset luminosity of dusty mass loss in population-II red giant stars. In this paper we present VISIR@VLT MIR 8.6 micron imaging of 47Tuc, centre of attention of a number of space-based Spitzer observations and studies. The VISIR high resolution (diffraction limited) observations allow excellent matching to existing optical Hubble space telescope catalogues. The optical-MIR coverage of the inner 1.15 arcmin of the cluster provide the cleanest possible, blending-free, sampling of the upper 3 magnitudes of the giant branch. Our diagrams show no evidence of faint giants with MIR-excess. A combined NIR-MIR diagram further confirms the near absence of dusty red giants. Dusty red giants and asymptotic giant stars are confined to the 47Tuc long period variables population. In particular, dusty red giants are limited to the upper one 8.6 micron magnitude below the giant branch tip. This particular luminosity level corresponds to ~1000 solar luminosity, suggested in previous determinations to mark the onset of dusty mass-loss. Interestingly, at this luminosity level, we detect a small deviation between the colours of red giants and the theoretical isochrones., Comment: Accepted for publication in A&A

Published
2011
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146. Stellar populations in the Phoenix dwarf galaxy

Author

Enrico Valerio Held, Saviane, I., and Momany, Y.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We have obtained deep BVI CCD photometry of Phoenix, a galaxy considered a transition case between dwarf spheroidal and dwarf irregular galaxies. A comparison of our data with the RGBs of Galactic globular clusters gives a mean metal abundance [Fe/H] = -1.81+/-0.10 dex. The presence of an intrinsic color dispersion in the upper red RGB suggests an abundance range of about 0.5 dex, although a range in age may also affect the RGB width. For the first time, a HB has been revealed at V~23.8. The HB is predominantly red yet moderately extended to the blue, which indicates the presence of a significant population with age comparable to that of old halo GGCs. This HB morphology in a metal-poor system indicates a mild "second parameter" effect. From the mean level of the HB we derived a true distance modulus 23.21+/-0.08, in good agreement with the distance modulus 23.04+/-0.07 estimated from the cutoff of the RGB at I~23.1. We find a radial gradient in the HB morphology, and our CMDs show a small number of stars above the RGB tip, that most likely are AGB stars of an intermediate age population. Their number indicates that the fraction of intermediate age population in Phoenix is approximately 30-40%. A young stellar population is definitely present in Phoenix, consistent with a star formation episode started at least 0.6 Gyr ago, up to 1x10^{8} yr ago. Both young stars and AGB stars are centrally concentrated, which indicates that recent star formation preferentially occurred in the inner galaxy regions. In many respects, Phoenix appears not dissimilar from dwarf spheroidal galaxies in the Local Group., 14 pages, 13 figures, accepted for publication in Astronomy and Astrophysics (main journal)

Published
1999

147. High Resolution HDS/SUBARU chemical abundances of the young stellar cluster Palomar 1

Author

Monaco, L., Saviane, I., Correnti, M., Bonifacio, P., Geisler, D., Monaco, L., Saviane, I., Correnti, M., Bonifacio, P., and Geisler, D.

Abstract

Context. Palomar\,1 is a peculiar globular cluster (GC). It is the youngest Galactic GC and it has been tentatively associated to several of the substructures recently discovered in the Milky Way (MW), including the Canis Major (CMa) overdensity and the Galactic Anticenter Stellar Structure (GASS). Aims. In order to provide further insights into its origin, we present the first high resolution chemical abundance analysis for one red giant in Pal\,1. Methods. We obtained high resolution (R=30000) spectra for one red giant star in Pal\,1 using the High Dispersion Spectrograph (HDS) mounted at the SUBARU telescope. We used ATLAS-9 model atmospheres coupled with the SYNTHE and WIDTH calculation codes to derive chemical abundances from the measured line equivalent widths of 18 among $\alpha$, Iron-peak, light and heavy elements. Results. The Palomar~1 chemical pattern is broadly compatible to that of the MW open clusters population and similar to disk stars. It is, instead, remarkably different from that of the Sagittarius (Sgr) dwarf spheroidal galaxy. Conclusions. If Pal\,1 association with either CMa or GASS will be confirmed, this will imply that these systems had a chemical evolution similar to that of the Galactic disk., Comment: 13 pages, 9 figures, 5 tables. Accepted for publication in Astronomy and Astrophysics. Minor changes in the text

Published
2010
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148. MAIN-SEQUENCE STAR POPULATIONS IN THE VIRGO OVERDENSITY REGION

Author

Jerjen, H., primary, Da Costa, G. S., additional, Willman, B., additional, Tisserand, P., additional, Arimoto, N., additional, Okamoto, S., additional, Mateo, M., additional, Saviane, I., additional, Walsh, S., additional, Geha, M., additional, Jordán, A., additional, Olszewski, E., additional, Walker, M., additional, Zoccali, M., additional, and Kroupa, P., additional

Published
2013
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150. Deep Impact: Observation from a worldwide earth-based campaign

Author

Meech, K.J., Ageorges, N., A'Hearn, M.F., Arpigny, C., Ates, A., Aycock, J., Bagnulo, S., Bailey, J., Barber, R., Barrera, L., Barrena, R., Bauer, J.M., Belton, M.J.S., Bensch, F., Bhattacharya, B., Biver, N., Blake, G., Bockelee-Morvan, D., Boehnhardt, H., Bonev, B.P., Bonev, T., Buie, M.W., Burton, M.G., Butner, H.M., Cabanac, R., Campbell, R., Campins, H., Capria, M.T., Carroll, T., Chaffee, F., Charnley, S.B., Cleis, R., Coates, A., Cochran, A., Colom, P., Conrad, A., Coulson, I.M., Crovisier, J., DeBuizer, J., Dekany, R., De Leon, J., Dello Russo, N., Delsanti, A., DiSanti, M., Drummond, J., Dundon, L., Etzel, P.B., Farnham, T.L., Feldman, P., Fernandez, Y.R., Filipovic, M.D., Fisher, S., Fitzsimmons, A., Fong, D., Fugate, R., Fujiwara, H., Fujiyoshi, T., Furusho, R., Fuse, T., Gibb, E., Groussin, O., Gulkis, S., Gurwell, M., Hadamcik, E., Hainaut, O., Harker, D., Harrington, D., Harwit, M., Hasegawa, S., Hergenrother, C.W., Hirst, P., Hodapp, K., Honda, M., Howell, E.S., Hutsemekers, D., Iono, O., Ip, W.-H., Jackson, W., Jehin, E., Jiang, Z.J., Jones, G.H., Jones, P.A., Kadono, T., Kamath, U.W., Kaufl, H.U., Kasuga, T., Kawakita, H., Kelley, M.S., Kerber, F., Kidger, M., Kinoshita, D., Knight, M., Lara, L., Larson, S.M., Lederer, S., Lee, C.-F., Levasseur-Regourd, A.C., Li, J.Y., Li, Q.-S., Licandro, J., Lin, Z.-Y., Lisse, C.M., LoCurto, G., Lovell, A.J., Lowry, S.C., Lyke, J., Lynch, D., Ma, J., Magee-Sauer, K., Maheswar, G., Manfroid, J., Marco, O., Martin, P., Melnick, G., Miller, S., Miyata, T., Moriarty-Schieven, G.H., Moskovitz, N., Mueller, B.E.A., Mumma, M.J., Muneer, S., Neufeld, D.A., Ootsubo, T., Osip, D., Pandea, S.K., Pantin, E., Paterno-Mahler, R., Patten, B., Penprase, B.E., Peck, A., Petitas, G., Pinilla-Alonso, N., Pittichova, J., Pompei, E., Prabhu, T.P., Qi, C., Rao, R., Rauer, H., Reitsema, H., Rodgers, S.D., Rodriguez, P., Ruane, R., Ruch, G., Rujopakarn, W., Sahu, D.K., Sako, S., Sakon, I., Samarasinha, N., Sarkissian, J.M., Saviane, I., Schirmer, M., Schultz, P., Schulz, R., Seitzer, P., Sekiguchi, T., Selman, F., Serra-Ricart, M., Sharp, R., Snell, R.L., Snodgrass, C., Stallard, T., Stecklein, G., Sterken, C., Stuwe, J.A., Sugita, S., Sumner, M., Suntzeff, N., Swaters, R., Takakuwa, S., Takato, N., Thomas-Osip, J., Thompson, E., Tokunaga, A.T., Tozzi, G.P., Tran, H., Troy, M., Trujillo, C., Van Cleve, J., Vasundhara, R., Vazquez, R., Vilas, F., Villanueva, G., Von Braun, K., Vora, P., Wainscoat, R.J., Walsh, K., Watanabe, J., Weaver, H.A., Weaver, W., Weiler, M., Weissman, P.R., Welsh, W.F., Wilner, D., Wolk, S., Womack, M., Wooden, D., Woodney, L.M., Woodward, C., Wu, Z.-Y., Wu, J.-H., Yamashita, T., Yang, B., Yang, Y.-B., Yokogawa, S., Zook, A.C., Zauderer, A., Zhao, X., Zhou, X., Zucconi, J.-M., Meech, K.J., Ageorges, N., A'Hearn, M.F., Arpigny, C., Ates, A., Aycock, J., Bagnulo, S., Bailey, J., Barber, R., Barrera, L., Barrena, R., Bauer, J.M., Belton, M.J.S., Bensch, F., Bhattacharya, B., Biver, N., Blake, G., Bockelee-Morvan, D., Boehnhardt, H., Bonev, B.P., Bonev, T., Buie, M.W., Burton, M.G., Butner, H.M., Cabanac, R., Campbell, R., Campins, H., Capria, M.T., Carroll, T., Chaffee, F., Charnley, S.B., Cleis, R., Coates, A., Cochran, A., Colom, P., Conrad, A., Coulson, I.M., Crovisier, J., DeBuizer, J., Dekany, R., De Leon, J., Dello Russo, N., Delsanti, A., DiSanti, M., Drummond, J., Dundon, L., Etzel, P.B., Farnham, T.L., Feldman, P., Fernandez, Y.R., Filipovic, M.D., Fisher, S., Fitzsimmons, A., Fong, D., Fugate, R., Fujiwara, H., Fujiyoshi, T., Furusho, R., Fuse, T., Gibb, E., Groussin, O., Gulkis, S., Gurwell, M., Hadamcik, E., Hainaut, O., Harker, D., Harrington, D., Harwit, M., Hasegawa, S., Hergenrother, C.W., Hirst, P., Hodapp, K., Honda, M., Howell, E.S., Hutsemekers, D., Iono, O., Ip, W.-H., Jackson, W., Jehin, E., Jiang, Z.J., Jones, G.H., Jones, P.A., Kadono, T., Kamath, U.W., Kaufl, H.U., Kasuga, T., Kawakita, H., Kelley, M.S., Kerber, F., Kidger, M., Kinoshita, D., Knight, M., Lara, L., Larson, S.M., Lederer, S., Lee, C.-F., Levasseur-Regourd, A.C., Li, J.Y., Li, Q.-S., Licandro, J., Lin, Z.-Y., Lisse, C.M., LoCurto, G., Lovell, A.J., Lowry, S.C., Lyke, J., Lynch, D., Ma, J., Magee-Sauer, K., Maheswar, G., Manfroid, J., Marco, O., Martin, P., Melnick, G., Miller, S., Miyata, T., Moriarty-Schieven, G.H., Moskovitz, N., Mueller, B.E.A., Mumma, M.J., Muneer, S., Neufeld, D.A., Ootsubo, T., Osip, D., Pandea, S.K., Pantin, E., Paterno-Mahler, R., Patten, B., Penprase, B.E., Peck, A., Petitas, G., Pinilla-Alonso, N., Pittichova, J., Pompei, E., Prabhu, T.P., Qi, C., Rao, R., Rauer, H., Reitsema, H., Rodgers, S.D., Rodriguez, P., Ruane, R., Ruch, G., Rujopakarn, W., Sahu, D.K., Sako, S., Sakon, I., Samarasinha, N., Sarkissian, J.M., Saviane, I., Schirmer, M., Schultz, P., Schulz, R., Seitzer, P., Sekiguchi, T., Selman, F., Serra-Ricart, M., Sharp, R., Snell, R.L., Snodgrass, C., Stallard, T., Stecklein, G., Sterken, C., Stuwe, J.A., Sugita, S., Sumner, M., Suntzeff, N., Swaters, R., Takakuwa, S., Takato, N., Thomas-Osip, J., Thompson, E., Tokunaga, A.T., Tozzi, G.P., Tran, H., Troy, M., Trujillo, C., Van Cleve, J., Vasundhara, R., Vazquez, R., Vilas, F., Villanueva, G., Von Braun, K., Vora, P., Wainscoat, R.J., Walsh, K., Watanabe, J., Weaver, H.A., Weaver, W., Weiler, M., Weissman, P.R., Welsh, W.F., Wilner, D., Wolk, S., Womack, M., Wooden, D., Woodney, L.M., Woodward, C., Wu, Z.-Y., Wu, J.-H., Yamashita, T., Yang, B., Yang, Y.-B., Yokogawa, S., Zook, A.C., Zauderer, A., Zhao, X., Zhou, X., and Zucconi, J.-M.

Abstract

On 4 July 2005, many observatories around the world and in space observed the collision of Deep Impact with comet 9P/Tempel 1 or its aftermath. This was an unprecedented coordinated observational campaign. These data show that (i) there was new material after impact that was compositionally different from that seen before impact; (ii) the ratio of dust mass to gas mass in the ejecta was much larger than before impact; (iii) the new activity did not last more than a few days, and by 9 July the comet's behavior was indistinguishable from its pre-impact behavior; and (iv) there were interesting transient phenomena that may be correlated with cratering physics.

Published
2005

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