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Selected publications and links to the data:

Part I (from 2003 to date)

(see Part II for publications before 2003)

Reference

Contents


Torres-Zafra, J., Cellone, S.A., Buzzoni, A., Andruchow, I., Portilla, J.G.:
"Redshift determination of the BL Lac object 3C 66A by the detection of its host galaxy cluster at z = 0.340", 2017, MNRAS, in press

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The BL Lac object 3C 66A is one of the most luminous extragalactic sources at TeV-rays (VHE, i.e. E >100 GeV) of unknown redshift. According to GEMINI observations we found spectroscopic evidence of two galaxy groups along the blazar's line of sight: one at z~0.020 and a second one at z~0.340. The blazar’s spectrum shows broad absorption features that we identify as arising in the intergalactic medium from a redshift z3C66A < 0.33. As a consequence, we propose that 3C 66A is hosted in a galaxy that belongs to a cluster at z = 0.340.

 

Annibali, F., Tosi, M., Romano, D., Buzzoni, A., Cusano, F., Fumana, M., Marchetti, A., Mignoli, M., Pasquali, A., Aloisi, A.:
"Planetary Nebulae and HII Regions in the Starburst Irregular Galaxy NGC 4449 from LBT MODS Data", 2017, The Astrophysical Journal, 843, 20

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We present deep 3500-10000 Å spectra of HII regions and planetary nebulae (PNe) in the starburst irregular galaxy NGC 4449, acquired with the Multi Object Double Spectrograph at the Large Binocular Telescope. Using the "direct" method, we derived the abundance of He, N, O, Ne, Ar, and S in six H II regions and in four PNe in NGC 4449. This is the first case of PNe studied in a starburst irregular outside the Local Group.

 

Buzzoni, A., Fan, S., Frueh, C., Altavilla, G., Foppiani, I., Micheli, M., Nomen, J., and Sanchez-Ortiz, N.:
"The puzzling case of the deep-space debris WT1190F: a test bed for advanced SSA techniques", 2016, Proc. of the Final Stardust Conference, ESA ESTEC, Noordwijk, The Netherlands (in press)

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We report on somewhat unique photometric and spectroscopic observations of the deep-space debris WT1190F. An analysis is in progress to assess the two prevailing candidates to WT1190F's identity, namely the Athena II upper stage of the Lunar Prospector mission, and the ascent stage of the Apollo 10 lunar module (LEM LM-4) "Snoopy", by comparing observations with the synthetic photometry from accurate mock-up modeling and reflectance rendering.

 

Fan, S., Frueh, C., and Buzzoni, A.:
"A Light Curve Simulation of The Apollo Lunar Ascent Module", 2016, AIAA/AAS Astrodynamics Specialist Conference, AIAA SPACE Forum, (AIAA 2016-5504), Long Beach, California

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The deep-space debris WT1190F, which entered Earth atmosphere off the Sri Lanka coast, last Nov 13, 2015, has been imposing to the worldwide SSA community as an outstanding opportunity to effectively assess origin and physical nature of such extemporary impactors and appraise their potential threat for Earth. During the event, astrometric signature of the object was obtained from Loiano, Italy and DEIMOS, Spain. As a primary candidate, generating the light curve of the long last Apollo 10 Lunar ascent module (call sign “Snoopy”) is useful in terms of examining the confidence level of the candidate.

 

Buzzoni, A., Altavilla, G., and Galleti, S.:
"Optical tracking of deep-space spacecraft in Halo L2 orbits and beyond: the Gaia mission as a pilot case", 2016, Advances in Space Research

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We tackle the problem of accurate optical tracking of distant man-made probes, on Halo orbit around the Earth-Sun libration point L2 and beyond, along interplanetary transfers. The improved performance of on-target tracking, especially when observing with small-class telescopes is assessed providing a general estimate of the expected S/N ratio in spacecraft detection. The on-going Gaia mission is taken as a pilot case for our analysis, reporting on fresh literature and original optical photometry and astrometric results.

 

Buzzoni, A.:
"Lick-index entanglement and biased diagnostic of stellar populations in galaxies", 2015, MNRAS, 449, 296

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The Lick-index spectrophotometric system is investigated in its inherent statistical and operational properties to ease a more appropriate use for astrophysical studies. Among others, the perturbing effect of [OIII]5007 and [NI]5199 forbidden gas emission on Fe5015 and Mgb absorption features is considered, and an updated correction scheme is proposed when using [OIII]5007 as a proxy to appraise Hβ residual emission. When applied to present-day elliptical galaxy population, the revised Hß scale leads, on average, to 20-30% younger age estimates.

 

Carraro, G., Buzzoni, A., Bertone, E., and Buson, L.:
"UB CCD photometry of the old, metal rich, open clusters NGC 6791, NGC 6819 and NGC 7142", 2013, AJ, 146, 128

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We report on a UV-oriented imaging survey in the fields of the old, metal-rich open clusters, NGC 6791, NGC 6819 and NGC 7142. Following a first discussion of NGC 6791 observations in an accompanying paper, here, we complete our analysis, also presenting for NGC 6819 and NGC 7142 the first-ever U CCD photometry. The color magnitude diagram of the three clusters is analyzed in detail, with special emphasis to the hot stellar component. We report, in this regard, one new extreme horizontal-branch star candidate in NGC 6791.

 

Buzzoni, A., Bertone, E., Carraro, G., and Buson, L.:
"Stellar lifetime and ultraviolet properties of the old metal-rich Galactic open cluster NGC6791: a pathway to understand the UV upturn of elliptical galaxies", 2012, ApJ, 749, 35

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The evolutionary properties of the old metal-rich Galactic open cluster NGC6791 are assessed, based on deep UB photometry and 2Mass JK data. For 4739 stars in the cluster, bolometric luminosity and effective temperature have been derived from theoretical (U-B) and (J-K) color fitting. The cluster appears to be a fairly good proxy of standard elliptical galaxies, although with significantly bluer infrared colors, a shallower 4000 Å Balmer break, and a lower Mg2 index.

 

Buzzoni, A.:
"Energetic constraints to chemo-photometric evolution of spiral galaxies", 2011, MNRAS, 415, 1155

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The problem of chemo-photometric evolution of late-type galaxies is dealt with relying on prime physical arguments of energetic self-consistency between chemical enhancement of galaxy mass, through nuclear processing inside stars, and luminosity evolution of the system. Chemical enhancement is assessed in terms of the so-called "yield metallicity" (Z), that is the metal abundance of processed mass inside stars, as constrained by the galaxy photometric history.

 

Buzzoni, A., Patelli, L., Bellazzini, M., Fusi Pecci, F., & Oliva, E.:
"Bolometric correction and spectral energy distribution of cool stars in Galactic clusters", 2010, MNRAS, 403, 1592

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We have investigated the relevant trend of the bolometric correction (BC) at the cool-temperature regime of red giant stars and its possible dependence on stellar metallicity. Our analysis relies on a wide sample of optical-infrared spectroscopic observations, along the 3500Å-2.5μm wavelength range, for a grid of 92 red giant stars in five (3 globular + 2 open) Galactic clusters, along the −2.2<[Fe/H]<+0.4 metallicity range.

 

Buzzoni, A., Bertone, E., & Chavez, M.:
"Snapshot metallicity estimate of resolved stellar systems through Lick Fe5270 diagnostic", 2009, Astrophysical Journal, 703, L127

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We outline a new method to derive a "snapshot" metallicity estimate of stellar systems (providing one resolves at least the brightest part of the CMD) just on the basis of low-resolution (i.e., 6-8 Å FWHM) spectroscopy of a small stellar sample. Our method relies on the Fe5270 Lick index measurements tracing the ubiquitous component of K-type giants. This makes the Fe5270 (max) estimate a robust and model-independent tracer of cluster [Fe/H], being particularly insensitive to the age of the stellar population.

 

Buzzoni, A., & Gónzalez-Lópezlira, R.A.:
"AGB Connection and Ultraviolet Luminosity Excess in Elliptical Galaxies", 2008, Astrophys. Journal, 686, 1007

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Relying on infrared surface brightness fluctuactions to trace AGB properties in a sample of elliptical galaxies in the Virgo and Fornax clusters, we assess the puzzling origin of the "UV-upturn" phenomenon, recently traced down to the presence of a hot horizontal branch (HB) stellar component. We find that the UV-upturn actually signals a profound change in the c-m diagram of stellar populations in elliptical galaxies, involving both the hot stellar component and red-giant evolution.

 

Buzzoni, A., Bertone, E., Chavez, M. & Rodriguez-Merino, L.H.:
"Population synthesis at short wavelengths and spectrophotometric diagnostic tools for galaxy evolution", 2007, an invited contribution to the intl. conference "New quests in stellar astrophysics. II: Ultraviolet properties of evolved stellar populations" (Puerto Vallarta, Mexico, 16-20/Apr/2007), eds. M. Chavez, E. Bertone, L.H. Rodriguez-Merino & D. Rosa-Gonzalez (Springer Verlag: Heidelberg), p.263.

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Taking advantage of recent important advances in the calculation of high-resolution spectral grids of stellar atmospheres at short-wavelengths, and their implementation for population synthesis models, we briefly review here some special properties of ultraviolet emission in SSPs, and discuss their potential applications for identifying and tuning up effective diagnostic tools to probe distinctive evolutionary properties of early-type galaxies and other evolved stellar systems.

 

Buzzoni, A.:
"Late stages of stellar evolution and their impact on spectrophotometric properties of galaxies", 2007, an invited contribution to the intl. conference "From Stars to Galaxies: Building the pieces to build up the Universe" (Venezia, Italy, 16-20/Oct/2006), ASP Conf. Series, no. 374, eds. A. Vallenari, R. Tantalo, L. Portinari and A. Moretti (ASP: San Francisco) p. 311

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The connection between AGB evolution of stellar populations and infrared vs. ultraviolet properties of the parent galaxies is reviewed relying on the updated lookout provided by population-synthesis theory. In particular, planetary-nebula events and hot horizontal-branch evolution are assessed in a unitary view to outline a plain general picture of galaxy spectrophotometric evolution. This will include a brief discussion of relevant phenomena such as the "UV upturn" in ellipticals and the stellar mass loss properties along the galaxy morphological sequence.

 

Cellone, S.A., Buzzoni, A.:
"The low-luminosity galaxy population in the NGC 5044 group", 2007, proc. of "Groups of Galaxies in the Nearby Universe", eds. I. Saviane, V. Ivanov and J. Borissova, ESO Astrophys. Symp.,(Springer Verlag: Heidelberg) p. 91

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Detailed surface photometry for 79 (mostly dwarf) galaxies in the NGC 5044 Group area is analysed, revealing the existence of different morphologies among objects originally classified as early-type dwarfs. Particularly, a significant fraction of bright dwarf "ellipticals" show a distinct bulge+disc structure, pointing to possible "harassed" disc galaxy evolution.

 

Buzzoni, A., Arnaboldi, M., Corradi, R.L.M.:
"Planetary nebulae as tracers of galaxy stellar populations", 2006, MNRAS, 368, 877.

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We address the general problem of the luminosity-specific planetary nebula (PN) number, defined as α = NPN/Lgal, and its relationship with age and metallicity of the parent stellar population. Our analysis relies on population synthesis models for SSPs and more elaborated galaxy models along the full star-formation range of the Hubble morphological sequence. This theoretical framework is compared with the updated census of the PN population in Local Group galaxies and external ellipticals in the Leo group, and the Virgo and Fornax clusters.

 

Buzzoni, A.:
"Photometric entropy of stellar populations and related diagnostic tools", 2005, Proc. of "Resolved Stellar Populations", eds. D. Valls-Gabaud & M. Chavez, ASP Conf. Ser. (ASP: San Francisco), in press.

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A confident assessment of the effective number and luminosity of stellar contributors in fully or partially unresolved aggregates, like globular clusters and distant galaxies can provide a very useful interpretative tool to properly assess the observational bias coming from crowding conditions or surface brightness fluctuations. These arguments have led us to introduce a new concept of "photometric entropy" of a stellar population, whose impact on different astrophysical aspects of cluster diagnostic has been reviewed here.

 

Fusi Pecci, F., Bellazzini, M., Buzzoni, A., De Simone, E., Federici, L., Galleti, S.:
"Massive young clusters in the disk of M31", 2005, Astron. Journal, 130, 554.

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We have studied the properties of a sample of 67 very blue and likely young massive clusters in M31, extracted from the Bologna Revised Catalog of globular clusters. These Blue Luminous Compact Clusters (BLCCs) are a significant fraction (> 15%) of the whole globular cluster system of M31. Their typical age turns out to be less than ~2 Gyr, while they probably are not so metal-poor as previously considered. The cluster sample distributes onto the outskirts of M31, sharing the kinematical properties of the thin, rapidly rotating disc component.

 

Buson, L.M., Buzzoni, A., Carraro, G., Bertone, E.:
"EHB stars in the Galactic open cluster NGC 6791: a Rosetta Stone to probe the UV-upturn phenomenon in giant ellipticals", 2006, Baltic Astronomy 15, 49.

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A new set of 13 UV-bright post-HB candidate stars in the field of the Galactic open cluster NGC 6791 have been discovered from TNG U,B imagery. Owing to its high metal content ([Fe/H]~0.4) and estimated age (t > 8 Gyr), this cluster represents the nearest ideal aggregate to reproduce the evolved stellar population giving rise to the UV-upturn phenomenon in Ellipticals and Spiral bulges.

 

Buzzoni, A.:
"Broad-band colors and overall photometric properties of template galaxy models from stellar population synthesis", 2005, MNRAS, 361, 725

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We present here a new set of evolutionary population synthesis models for template galaxies along the Hubble morphological sequence. The models, that account for the individual evolution of the bulge, disk, and halo components, provide basic morphological features, along with bolometric luminosity and color evolution (including Johnson/Cousins "UBVRcIcJHK", Gunn "gri", and Washington "CMT1T2" photometric systems) between 1 and 15 Gyr. Luminosity contribution from residual gas is also evaluated, both in terms of nebular continuum and Balmer-line enhancement.

 

Bertone, E., Chavez, M., Rodriguez-Merino, L., Buzzoni, A.:
"On age and metallicity of evolved stellar populations", 2005, proc. of "Resolved Stellar Populations", ASP Conf. Series., eds. M. Chavez and D. Valls-Gabaud, (ASP: San Francisco) in press.

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We analyze the applicability of updated stellar libraries and synthesis codes in determining the age and chemical composition of evolved stellar populations from their integrated UV spectra. Here we discuss the relevant case of two fundamental calibrators, namely the Sun and the galaxy M32.

 

Chavez, M., Bertone, E., Rodriguez-Merino, L., Buzzoni, A., Bressan, A.:
"Synthetic mid-UV indices of stars and Simple Stellar Populations", 2005, proc. of "Resolved Stellar Populations", ASP Conf. Series., eds. M. Chavez and D. Valls-Gabaud, (ASP: San Francisco) in press.

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Using the UVBLUE library we have computed all mid-UV spectroscopic indices as defined by Fanelli et al. (1990). We explore their behaviour in terms of the leading stellar parameters (Teff, log g, [Fe/H]) and also and quantify the effect of instrumental resolution. We also implemented the UVBLUE grid in two population synthesis codes (Buzzoni 1989; Bressan et al. 1994), producing a grid of integrated mid-UV spectra for SSPs over a wide range of age and metallicity.

 

Kinman, T.D., Bragaglia, A., Cacciari, A., Buzzoni, A., Spagna, A.:
"The Galactic halo towards the North Galactic Pole", 2005, proc. of "The Three Dimensional Universe with GAIA", ESA SP-576, eds. C. Turon, K.S. O'Flaherty and M.A.C. Perryman (ESA: Paris) p. 175

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We have used RR Lyrae and Blue HB stars as tracers of the old Galactic halo, in order to study the halo structure and the galactic rotation as a function of height above the plane. From the whole sample the motion appears to be significantly more retrograde than the samples in the solar neighborhood. However, the better statistics has now revealed the likely existence of two components, whose characteristics need an accurate analysis of systematic errors on the proper motions in order to be assessed in detail.

 

Cellone, S.A., Buzzoni, A.:
"The low-luminosity galaxy population in the NGC 5044 group", 2005, MNRAS, 356, 41.

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We present multicolour imaging for a sample of 33 dwarf and intermediate-luminosity galaxies in the field of the NGC 5044 Group, complemented with mid-resolution spectroscopy for a subsample of 13 objects. A revised membership and morphological classification is made for the galaxies in the sample and six new dSph candidates were also found. Kinematical data show no luminosity segregation for early-type galaxies and a much broader distribution of spirals.

 

Solano, E. et al. (with Buzzoni, A.):
"Gaudi: a preparatory archive for the COROT mission", 2005, Astron. Journal, 129, 547.

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The GAUDI database is a preparatory archive for the COROT space mission developed at LAEFF. It contains spectroscopic and photometric data together with inferred physical parameters for more than 1500 stars gathered since Jan 1998 in 6 years of observational campaign. In this paper, the main functionalities and characteristics of the system are described.

 

Buzzoni, A., Bertone, E., Rodriguez-Merino, L., Chavez, M.:
"Beyond the Lick Indices: the High-resolution Spectral Synthesis of Stellar Populations", 2005, proc. of the ESO workshop on "Multiwavelength Mapping of Galaxy Formation and Evolution", eds. R. Bender and A. Renzini, ESO Conf. Series (Springer: Heidelberg) p. 361

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Up-to-date theoretical SED of stellar populations at 2 Å FWHM resolution is obtained by coupling a new library of synthetic spectra from the ATLAS and NextGen atmosphere database with the Buzzoni population synthesis code. We briefly outline the current status of the project, aimed at settling a new theoretical framework of narrow-band spectrophotometric indices to study stellar populations of galaxies.

 

Buzzoni, A., Arnaboldi, M.:
"Planetary Nebulae as tracers of the Intergalactic stellar background: a population synthesis theoretical approach", 2004, ESO intl. Workshop on "Planetary Nebulae beyond the Milky Way". To appear on the ESO Astrophysics Symposia, eds. L. Stanghellini, J.R. Walsh & N.G. Douglas (Springer Verlag: Heidelberg), p. 355.

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Relying on original population synthesis models, we assess the relationship between the population of planetary nebulae (PNe) and a given parent stellar population from a theoretical point of view. A tentative application to the Virgo cluster allows us to place a lower limit at ~7% for the global B luminosity of the cluster provided by "loose" intergalactic stars.

 

Bertone, E., Buzzoni, A., Chavez, M., Rodriguez-Merino, L.H.:
"ATLAS vs. NextGen model atmospheres: a combined analysis of synthetic spectral energy distributions", 2004, Astron. Journal, 128, 829.

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An exhaustive critical appraisal of the two most popular theoretical codes for stellar atmosphere synthesis, i.e. Kurucz' ATLAS9 and Hauschildt et al.'s PHOENIX/NextGen.

 

Bertone, E., Buzzoni, A., Chavez, M., Rodriguez-Merino, L.:
"High-resolution spectral synthesis: 2 Å mapping of UV-optical emission of stellar populations", 2003, presented at the MPA workshop on "Stellar Populations 2003" - Garching, Germany 6-10 October 2003.
Proceedings are available in electronic form only at this Web address

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We explore, from the theoretical point of view, the spectral properties of SSPs in the ultraviolet wavelength range, shortward of the 4000 Å break. Our models rely on a new stellar library of high-resolution (2 Å FWHM) synthetic spectra, based on the Kurucz model atmospheres, coupled with the Buzzoni population synthesis code. Some preliminary results of our project aimed at singling out those spectral features that can selectively track age and metallicity in stellar aggregates are presented and briefly discussed.

 

Cellone, S.A., and Buzzoni, A.:
"La población de galaxias de baja luminosidad en el grupo de NGC 5044", 2003, memorias de la Reunión Anual de la Asociación Argentina de Astronomía, Buenos Aires, Argentina, 16-19/Sep/2002 -- Published on the Boletín de la Asociación Argentina de Astronomía, vol. 46, p. 93-94

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We present preliminary results of a systematic spectrophotometric study of the dwarf- and low-luminosity galaxy population (19.5 < B(T) < 15.5) in the group of NGC 5044. Our work aims at obtaining membership and morphological classification as well as color properties of this class of galaxies in the framework of more general dynamical and environmental study of the NGC 5044 group.

 

Chavez, M., Rodriguez-Merino, L.H., Bertone, E., Buzzoni, A.:
"Spectroscopic indices of stars: a theoretical approach", 2002, proc. of the Intl. Symp. on "Astrophysics Research and the Dialog between Science and Religion", Vatican Observatory,Eds. C.D. Impey and C.E. Petry (in press)

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A new grid of theoretical absorption indices based on the Kurucz library of synthetic spectra is presented. Models encompass the wavelength interval from 850 to 7000 Å, with an inverse resolution R = 50,000 (UV range) and 500,000 (optical). A total of 51 ultraviolet and optical narrow-band indices defined in the literature have been measured therefrom and calibrated in terms of the atmosphere parameters.

 

Kinman, T.D., Cacciari, C., Bragaglia, A., Buzzoni, A., Spagna, A.:
"The vertical structure of the halo rotation", 2003, proc. of the JENAM workshop on "Galactic and Stellar Dynamics" - Porto, Portugal 3-6 September 2002, Eds. C. M. Boily, P. Pastsis, S. Portegies Zwart, R. Spurzem & C. Theis, EAS Publ. Series, 10, 115

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New GSC-II proper motions of RR Lyrae and Blue Horizontal Branch (BHB) stars near the North Galactic Pole are used to show that the Galactic Halo 5 kpc above the Plane has a significantly retrograde galactic rotation.

 

Buzzoni, A.:
"UV properties and evolution of high-redshift galaxies", 2003, proc. of the ASP Conf. Ser. no. 297 "Star Formation through Time" - Granada, Spain 24-28/Sep/2002, Eds. E. Perez, R. Gonzalez-Delgado, G. Tenorio-Tagle (ASP: San Francisco), p. 471

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I assess the problem of morphological and photometric evolution of high-redshift galaxies in the ultraviolet wavelength range. My discussion will partly rely on a new set of template galaxy models, in order to infer the expected changes along the Hubble morphological sequence at the different cosmic epochs. The impact of evolution on the faint-end galaxy luminosity function at z~1 and beyond will also be evaluated and briefly discussed.

 

Rodriguez-Merino, L.H., Chavez, M., Bertone, E., Buzzoni, A.:
" An updated FUV-blue stellar library for modelling stellar systems", 2003, proc. of the ASP Conf. Ser. no. 297 "Star Formation through Time" - Granada, Spain 24-28/Sep/2002, Eds. E. Perez, R. Gonzalez-Delgado, G. Tenorio-Tagle (ASP: San Francisco), p. 237

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We present a new theoretical library of stellar spectra computed at high resolution (R = 50,000). The library covers the wavelength interval from 850 to 4750 Å, and spans a wide temperature range from 3000 K to 50,000 K across the whole MK types (from dwarf to super-giant stars) in the H-R diagram.

 

Bertone, E., Rodriguez-Merino, L.H., Chavez, M., Buzzoni, A.:
"A library of UV-optical high-resolution synthetic spectra for the study of stellar aggregates", 2003, proc. of "Galaxy Evolution: Theory and Observations" - Cozumel, Mexico 8-12 April 2002, Eds. V. Avila-Reese, C. Firmani, C. Frenk, & C. Allen, Rev.Mex. Astron. Astrophys. Conf. Ser., 17, 91

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A synthetic spectral library for stars in the temperature range between 4,000 and 50,000 K is presented. Model grid covers the wavelength interval from 912 to 7000 Å at inverse resolution R = 50,000 (in the 912 to 4500 Å interval) and R = 500,000 otherwise. Calculations relied on the Kurucz original code ATLAS. The model grid spans metallicity from [M/H] = -2.0 to +0.5 and log g from 0.0 to 5.0 dex. This is currently the most extended theoretical library available in the literature at such high resolution.

 

 
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