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Photometric and Spectroscopic Monitoring of the sdBV star PG 1605+072: The Multi-Site Spectroscopic Telescope (MSST) Project  [PDF]
U. Heber,S. Dreizler,S. L. Schuh,S. O'Toole,C. S. Jeffery
Physics , 2002,
Abstract: A small fraction of subluminous B stars show short-period, multiperiodic light variations and form the new class of pulsating star known as EC 14026 variables, after the prototype. The Multi-Site Spectroscopic Telescope (MSST) is a virtual instrument and is also the name of a collaboration that aims to open up a new observational window to provide access to a mode identification for and an asteroseismological analysis of the pulsating sdB star PG 1605+072. Although the primary aim is to obtain time resolved spectroscopy it also includes the most extended photometric monitoring campaign for PG 1605+072.
A photometric and spectroscopic survey of solar twin stars within 50 parsecs of the Sun: I. Atmospheric parameters and color similarity to the Sun  [PDF]
G. F. Porto de Mello,R. da Silva,L. da Silva,R. V. de Nader
Physics , 2013, DOI: 10.1051/0004-6361/201322277
Abstract: Solar twins and analogs are fundamental in the characterization of the Sun's place in the context of stellar measurements, as they are in understanding how typical the solar properties are in its neighborhood. They are also important for representing sunlight observable in the night sky for diverse photometric and spectroscopic tasks, besides being natural candidates for harboring planetary systems similar to ours and possibly even life-bearing environments. We report a photometric and spectroscopic survey of solar twin stars within 50 pc of the Sun. Hipparcos absolute magnitudes and (B-V)_Tycho colors were used to define a 2 sigma box around the solar values, where 133 stars were considered. Additional stars resembling the solar UBV colors in a broad sense, plus stars present in the lists of Hardorp, were also selected. All objects were ranked by a color-similarity index with respect to the Sun, defined by uvby and BV photometry. Moderately high-resolution, high-S/N spectra were used for a subsample of equatorial-southern stars to derive Teff, log g, and [Fe/H] with average internal errors better than 50 K, 0.20 dex, and 0.08 dex, respectively. Ages and masses were estimated from theoretical HR diagrams. The color-similarity index proved very successful. We identify and rank new excellent solar analogs, which are fit to represent the Sun in the night sky. Some of them are faint enough to be of interest for moderately large telescopes. We also identify two stars with near-UV spectra indistinguishable from the Sun's. We present five new "probable" solar twin stars, besides five new "possible" twins. Masses and ages for the best solar twin candidates lie very close to the solar values, but chromospheric activity levels range somewhat. We propose that the solar twins be emphasized in the ongoing searches for extra-solar planets and SETI searches.
POISSON project - II - A multi-wavelength spectroscopic and photometric survey of young protostars in L 1641  [PDF]
A. Caratti o Garatti,R. Garcia Lopez,S. Antoniucci,B. Nisini,T. Giannini,J. Eisloeffel,T. P. Ray,D. Lorenzetti,S. Cabrit
Physics , 2011, DOI: 10.1051/0004-6361/201117781
Abstract: Characterising stellar and circumstellar properties of embedded young stellar objects (YSOs) is mandatory for understanding the early stages of the stellar evolution. This task requires the combination of both spectroscopy and photometry, covering the widest possible wavelength range, to disentangle the various protostellar components and activities. As part of the POISSON project, we present a multi-wavelength spectroscopic and photometric investigation of embedded YSOs in L1641, aimed to derive the stellar parameters and evolutionary stages and to infer their accretion properties. Our database includes low-resolution optical-IR spectra from the NTT and Spitzer (0.6-40 um) and photometric data covering a spectral range from 0.4 to 1100 um, which allow us to construct the YSOs spectral energy distributions (SEDs) and to infer the main stellar parameters. The SED analysis allows us to group our 27 YSOs into nine Class I, eleven Flat, and seven Class II objects. However, on the basis of the derived stellar properties, only six Class I YSOs have an age of ~10^5 yr, while the others are older 5x10^5-10^6 yr), and, among the Flat sources, three out of eleven are more evolved objects (5x10^6-10^7 yr), indicating that geometrical effects can significantly modify the SED shapes. Inferred mass accretion rates (Macc) show a wide range of values (3.6x10^-9 to 1.2x10^-5 M_sun yr^-1), which reflects the age spread observed in our sample. Average values of mass accretion rates, extinction, and spectral indices decrease with the YSO class. The youngest YSOs have the highest Macc, whereas the oldest YSOs do not show any detectable jet activity in either images and spectra. We also observe a clear correlation among the YSO Macc, M*, and age, consistent with mass accretion evolution in viscous disc models.
Photometric and spectroscopic investigation of TW Draconis  [PDF]
M. Zejda,M. Wolf,M. Slechta,Z. Mikulasek,J. Zverko,P. Svoboda,J. Krticka,J. Janik,H. Bozic
Physics , 2010,
Abstract: Context. TW Draconis is one of the best studied Algol-type eclipsing binaries. There is significant evidence for miscellaneous physical processes between interacting binary components manifesting themselves by period and light curve changes. Aims. Obtaining new set of photometric and spectroscopic observations, we analysed them together with the older spectroscopic and photometric data to build model of this eclipsing system with respect to observed changes of O-C diagram and light curve. Methods. Reduction of new spectra was carried out in the IRAF and SPEFO programs. Radial velocities were determined manually using SPEFO, by CCF using the Zverko's code and from the program KOREL. Orbital elements were derived with the FOTEL program and via disentangling with KOREL. The final combined solution was obtained with the programs PHOEBE and FOTEL. Results. Photometry shows small irregularities in light curves as a results of pulsating of one component and spot activity. Using net of KOREL outputs we found the mass ratio q=0.405(3).We confirm the presence of stellar matter around the primary. Even after subtraction of ADS 9706B influence, light curve solutions show third light in the system. Models in FOTEL and Phoebe are presented. Conclusions. TW Dra is an astrophysically very interesting eclipsing binary. Future combination of interferometry, spectroscopy, and photometry is promising. It could definitely confirm the hypothesis of quadruple system for TW Dra and explain behaviour of this system in complex.
Photometric and Spectroscopic Study of Abell 0671  [PDF]
Zhizheng Pan,Qirong Yuan,Xu Kong,Dongxin Fan,Xu Zhou,Xuanbin Lin
Physics , 2011, DOI: 10.1111/j.1365-2966.2011.19907.x
Abstract: In this paper we present a photometric and spectroscopic study of the nearby galaxy cluster Abell 0671 (A671) with 15 intermediate-band filters in the Beijing-Arizona-Taiwan-Connecticut (BATC) system and the Sloan Digital Sky Survey (SDSS) data. The photometric redshift technique is applied to the galaxy sample for further membership determination. After the color-magnitude relation is taken into account, 97 galaxies brighter than h_batc=19.5 mag are selected as new member galaxies. Based on the enlarged sample of cluster galaxies, spatial distribution, dynamics of A671 are investigated. The substructures of A671 are well shown by the sample of bright members, but it appears less significant based on the enlarged sample, which is mainly due to larger uncertainties in the light-of-sight velocities of the newly-selected faint members. The SDSS r-band luminosity function of A671 is flat at faint magnitudes, with the faint end slope parameter alpha=-1.12. The SDSS spectra allow us to investigate the star formation history of bright cluster galaxies, and the galaxies in the core region are found to be older than those in the outskirts. No environmental effect is found for metallicities of the early-type galaxies (ETGs). The positive correlation between age and stellar mass supports the downsizing scenario. By comparing ETG absorption-line indices with the state-of-art stellar population models, we derive the relevant parameters of simple stellar population (such as age, [Fe/H], [Mg/Fe], [C/Fe], [N/Fe], and [Ca/Fe]). The ETGs at cluster center tend to have smaller hb indices, indicating that central ETGs are likely to be older. The distribution of total metallicity indicator, [MgFe]', does not show any environmental effects. The relations between the simple stellar population parameters and velocity dispersion in A671 are in good agreement with previous studies.
Quantifying Photometric Redshift Errors in the Absence of Spectroscopic Redshifts  [PDF]
Ryan F. Quadri,Rik J. Williams
Physics , 2009, DOI: 10.1088/0004-637X/725/1/794
Abstract: Much of the science that is made possible by multiwavelength redshift surveys requires the use of photometric redshifts. But as these surveys become more ambitious, and as we seek to perform increasingly accurate measurements, it becomes crucial to take proper account of the photometric redshift uncertainties. Ideally the uncertainties can be directly measured using a comparison to spectroscopic redshifts, but this may yield misleading results since spectroscopic samples are frequently small and not representative of the parent photometric samples. We present a simple and powerful empirical method to constrain photometric redshift uncertainties in the absence of spectroscopic redshifts. Close pairs of galaxies on the sky have a significant probability of being physically associated, and therefore of lying at nearly the same redshift. The difference in photometric redshifts in close pairs is therefore a measure of the redshift uncertainty. Some observed close pairs will arise from chance projections along the line of sight, but it is straightforward to perform a statistical correction for this effect. We demonstrate the technique using both simulated data and actual observations, and discuss how its usefulness can be limited by the presence of systematic photometric redshift errors. Finally, we use this technique to show how photometric redshift accuracy can depend on galaxy type.
On the compared accuracy and reliability of spectroscopic and photometric redshift measurements  [PDF]
Alberto Fernandez-Soto,Kenneth M. Lanzetta,Hsiao-Wen Chen,Sebastian M. Pascarelle,Noriaki Yahata
Physics , 2000, DOI: 10.1086/321777
Abstract: We present a comparison between the spectroscopic catalog of the HDF recently published by Cohen et al and the redshifts measured by our group for those objects using photometric techniques. We perform this comparison in order to characterize the errors associated to the photometric redshift technique. The spectroscopic sample includes over 140 objects in the HDF proper, representing the deepest, cleanest, most complete spectroscopic catalog ever compiled. We study each object for which our redshift and the one measured by Cohen et al disagree. In most cases the photometric evidence is strong enough to call for a careful review of the spectroscopic values, as they seem to be in error. It is possible to characterize the systematic errors associated to our technique, which when combined with the photometric errors allow us to obtain complete information on the redshift of each galaxy and its associated confidence interval, regardless of apparent magnitude. One of the main conclusions of this study is that, to date, all the redshifts from our published catalog that have been checked have been shown to be correct (within the stated confidence limits). This implies that our galaxy template set is a fair representation of the galaxy population at all redshifts (0
Photometric and spectroscopic variations of the Be star HD 112999  [PDF]
M. A. Corti,R. C. Gamen,Y. J. Aidelman,G. A. Ferrero,W. A. Weidmann
Physics , 2013,
Abstract: Be objects are stars of B spectral type showing lines of the Balmer series in emission. The presence of these lines is attributed to the existence of an extended envelope, disk type, around them. Some stars are observed in both the Be and normal B-type spectroscopic states and they are known as transient Be stars. In this paper we show the analysis carried out on a new possible transient Be star, labelled HD 112999, using spectroscopic optical observations and photometric data.
Spectroscopic and Photometric Observations of Kepler Asteroseismic Targets  [PDF]
J. Molenda-Zakowicz,M. Jerzykiewicz,G. Kopacki,A. Frasca,G. Catanzaro,D. W. Latham,E. Niemczura,A. Narwid,M. Steslicki,T. Arentoft,J. Kubat,D. Drobek,W. Dimitrow
Physics , 2012, DOI: 10.1063/1.3246557
Abstract: We summarize our ground-based program of spectroscopic and photometric observations of the asteroseismic targets of the Kepler space telescope. We have already determined atmospheric parameters, projected velocity of rotation, and radial velocity of 62 Kepler asteroseismic targets and 33 other stars in the Kepler field of view. We discovered six single-lined and two double-lined spectroscopic binaries, we determined the interstellar reddening for 29 stars in the Kepler field of view, and discovered three delta Sct, two gamma Dor and 14 other variable stars in the field of NGC 6866.
Completeness in Photometric and Spectroscopic Searches for Clusters  [PDF]
Martin White,C. S. Kochanek
Physics , 2001, DOI: 10.1086/340944
Abstract: We investigate, using simulated galaxy catalogues, the completeness of searches for massive clusters of galaxies in redshift surveys or imaging surveys with photometric redshift estimates, i.e. what fraction of clusters (M>10^14/h Msun) are found in such surveys. We demonstrate that the matched filter method provides an efficient and reliable means of identifying massive clusters even when the redshift estimates are crude. In true redshift surveys the method works extremely well. We demonstrate that it is possible to construct catalogues with high completeness, low contamination and both varying little with redshift.
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