scholarly journals The Distribution of Main Belt Asteroids with Featureless Spectra from the Sloan Digital Sky Survey Photometry

2009 ◽  
Vol 5 (S263) ◽  
pp. 237-239
Author(s):  
Anderson O. Ribeiro ◽  
Fernando Roig
Keyword(s):  
Spectroscopic Data ◽  
Moving Objects ◽  
Photometric Data ◽  
Sloan Digital Sky Survey ◽  
Spectral Slope ◽  
Main Belt ◽  
Absorption Bands ◽  
Sky Survey ◽  
The Mean

AbstractIn this work, we propose to analyse the existence of possible correlations between the taxonomic classes of asteroids showing featureless spectra –i.e. a flat continuum with no absorption bands– and their orbital properties. We compute the mean spectral slope of 14 753 asteroids using the photometric data from the Sloan Digital Sky survey Moving Objects Catalog (SDSS-MOC4). Although the quality of these data is not comparable in resolution to the spectroscopic data, the amount of observations in the SDSS-MOC4 is more than 20 times larger that in the available spectral databases. This allows us to obtain a statistically significant result.

scholarly journals A catalogue of Locus Algorithm pointings for optimal differential photometry for 23 779 quasars

2020 ◽  
Vol 498 (3) ◽  
pp. 3720-3729
Author(s):  
Oisín Creaner ◽  
Kevin Nolan ◽  
Niall Smith ◽  
David Grennan ◽  
Eugene Hickey
Keyword(s):  
Time Scale ◽  
Figure Of Merit ◽  
Target Object ◽  
Sloan Digital Sky Survey ◽  
Field Of View ◽  
Computing Paradigm ◽  
Sky Survey ◽  
Differential Photometry ◽  
Suitable Reference

ABSTRACT This paper presents a catalogue of optimized pointings for differential photometry of 23 779 quasars extracted from the Sloan Digital Sky Survey (SDSS) Catalogue and a Score for each indicating the quality of the Field of View (FoV) associated with that pointing. Observation of millimagnitude variability on a time-scale of minutes typically requires differential observations with reference to an ensemble of reference stars. For optimal performance, these reference stars should have similar colour and magnitude to the target quasar. In addition, the greatest quantity and quality of suitable reference stars may be found by using a telescope pointing which offsets the target object from the centre of the FoV. By comparing each quasar with the stars which appear close to it on the sky in the SDSS Catalogue, an optimum pointing can be calculated, and a figure of merit, referred to as the ‘Score’ is calculated for that pointing. Highly flexible software has been developed to enable this process to be automated and implemented in a distributed computing paradigm, which enables the creation of catalogues of pointings given a set of input targets. Applying this technique to a sample of 40 000 targets from the fourth SDSS quasar catalogue resulted in the production of pointings and Scores for 23 779 quasars based on their magnitudes in the SDSS r-band. This catalogue is a useful resource for observers planning differential photometry studies and surveys of quasars to select those which have many suitable celestial neighbours for differential photometry.

scholarly journals The absorption spectra of halogens and inter-halogen compounds in solution in carbon tetrachloride

1929 ◽  
Vol 124 (795) ◽  
pp. 604-616 ◽  
Keyword(s):  
Absorption Spectrum ◽  
Carbon Tetrachloride ◽  
Absorption Spectra ◽  
Spectroscopic Data ◽  
Chemical Interaction ◽  
Chemical Compounds ◽  
Absorption Bands ◽  
Halogen Compounds ◽  
Inert Solvent ◽  
The Mean

When two solutions are mixed the absorption spectrum of the new solution will be the mean of those of the separate solutions provided that no chemical interaction occures. The mere fact of a departure from additivity does not, however, necessarily denote the formation of true chemical compounds. The solute or solutes may undergo solvation, loosely bound aggregates may occur, and even when marked deviations from the simple law of mixtures are observed it is rarely possible to prove the quantitative formation of a given chemical compound from spectroscopic data alone. The above considerations apply with some force to the problem of the absorption spectra of halogens and inter-halogen compounds in an inert solvent. The three elements show perfectly characteristic absorption bands, they are known to interact with the formation of some quite stable compounds, some relatively stable compounds, and some apparently very unstable compounds.

scholarly journals Identifying Circumgalactic Medium Absorption in QSO Spectra: A Bayesian Approach

2021 ◽  
Vol 923 (1) ◽  
pp. 44
Author(s):  
Jennifer E. Scott ◽  
Emileigh S. Shoemaker ◽  
Colin D. Hamill
Keyword(s):  
Bayesian Methods ◽  
Statistical Approach ◽  
Hubble Space Telescope ◽  
Spectroscopic Studies ◽  
Photometric Data ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
The Galaxy ◽  
Circumgalactic Medium

Abstract We present a study of candidate galaxy–absorber pairs for 43 low-redshift QSO sightlines (0.06 < z < 0.85) observed with the Hubble Space Telescope/Cosmic Origins Spectrograph that lie within the footprint of the Sloan Digital Sky Survey with a statistical approach to match absorbers with galaxies near the QSO lines of sight using only the SDSS Data Release 12 photometric data for the galaxies, including estimates of their redshifts. Our Bayesian methods combine the SDSS photometric information with measured properties of the circumgalactic medium to find the most probable galaxy match, if any, for each absorber in the line-of-sight QSO spectrum. We find ∼630 candidate galaxy–absorber pairs using two different statistics. The methods are able to reproduce pairs reported in the targeted spectroscopic studies upon which we base the statistics at a rate of 72%. The properties of the galaxies comprising the candidate pairs have median redshift, luminosity, and stellar mass, all estimated from the photometric data, z = 0.13, L = 0.1L *, and log ( M * / M ⊙ ) = 9.7 . The median impact parameter of the candidate pairs is ∼430 kpc, or ∼3.5 times the galaxy virial radius. The results are broadly consistent with the high Lyα covering fraction out to this radius found in previous studies. This method of matching absorbers and galaxies can be used to prioritize targets for spectroscopic studies, and we present specific examples of promising systems for such follow-up.

scholarly journals Detecting neutral hydrogen at z ≳ 3 in large spectroscopic surveys of quasars

2020 ◽  
Vol 498 (2) ◽  
pp. 1951-1962
Author(s):  
Michele Fumagalli ◽  
Sotiria Fotopoulou ◽  
Laura Thomson
Keyword(s):  
Random Forest ◽  
Neutral Hydrogen ◽  
Sloan Digital Sky Survey ◽  
Broad Absorption Line ◽  
Quasar Spectra ◽  
Sky Survey ◽  
William Herschel ◽  
High Column

ABSTRACT We present a pipeline based on a random forest classifier for the identification of high column density clouds of neutral hydrogen (i.e. the Lyman limit systems, LLSs) in absorption within large spectroscopic surveys of z ≳ 3 quasars. We test the performance of this method on mock quasar spectra that reproduce the expected data quality of the Dark Energy Spectroscopic Instrument and the WHT (William Herschel Telescope) Enhanced Area Velocity Explorer surveys, finding ${\gtrsim}90{{\ \rm per\ cent}}$ completeness and purity for $N_{\rm H\,\rm{\small I}} \gtrsim 10^{17.2}~\rm cm^{-2}$ LLSs against quasars of g &lt; 23 mag at z ≈ 3.5–3.7. After training and applying our method on 10 000 quasar spectra at z ≈ 3.5–4.0 from the Sloan Digital Sky Survey (Data Release 16), we identify ≈6600 LLSs with $N_{\rm H\,\rm{\small I}} \gtrsim 10^{17.5}~\rm cm^{-2}$ between z ≈ 3.1 and 4.0 with a completeness and purity of ${\gtrsim}90{{\ \rm per\ cent}}$ for the classification of LLSs. Using this sample, we measure a number of LLSs per unit redshift of ℓ(z) = 2.32 ± 0.08 at z = [3.3, 3.6]. We also present results on the performance of random forest for the measurement of the LLS redshifts and H i column densities, and for the identification of broad absorption line quasars.

THE DISTRIBUTION OF STELLAR MASS-TO-LIGHT RATIO IN THE LOCAL UNIVERSE

2011 ◽  
Vol 20 (10) ◽  
pp. 2105-2108
Author(s):  
CHENG LI
Keyword(s):  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Distribution Models ◽  
Quantitative Characterization ◽  
Local Universe ◽  
Sky Survey ◽  
The Mean ◽  
Halo Occupation Distribution ◽  
Mass Functions

We have used the final data release of the Sloan Digital Sky Survey (SDSS) to estimate the projected autocorrelation function, wp(rp), for the stellar mass of galaxies, as well as their stellar light in the SDSS five photometric bands. All these quantities are robustly and precisely determined over scales 10h-1 kpc < rp < 30h-1 Mpc . Ratios of wp(rp) between two given wavebands are proportional to the mean color of correlated stars at rp from a randomly chosen star, while the ratio of stellar mass to luminosity autocorrelations measures an analogous mean stellar mass-to-light ratio (M*/L). These measurements provide a precise quantitative characterization of the well-known dependence of stellar populations on environment, which, when combined with accurate luminosity and stellar mass functions, is expected to provide a compact way to constrain Halo Occupation Distribution models that try to represent all the correlations in detail.

scholarly journals THE NINTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY

2012 ◽  
Vol 203 (2) ◽  
pp. 21 ◽  
Author(s):  
Christopher P. Ahn ◽  
Rachael Alexandroff ◽  
Carlos Allende Prieto ◽  
Scott F. Anderson ◽  
Timothy Anderton ◽  
...  
Keyword(s):  
Spectroscopic Data ◽  
Sloan Digital Sky Survey ◽  
Sky Survey ◽  
Data Release

scholarly journals Contribution of Gaia Sausage to the Galactic Stellar Halo Revealed by K Giants and Blue Horizontal Branch Stars from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, Sloan Digital Sky Survey, and Gaia

2022 ◽  
Vol 924 (1) ◽  
pp. 23
Author(s):  
Wenbo Wu ◽  
Gang Zhao ◽  
Xiang-Xiang Xue ◽  
Sarah A. Bird ◽  
Chengqun Yang
Keyword(s):  
Gaussian Mixture ◽  
Sloan Digital Sky Survey ◽  
Horizontal Branch ◽  
Integrals Of Motion ◽  
Eccentric Orbits ◽  
Horizontal Branch Stars ◽  
Sky Survey ◽  
Stellar Halo ◽  
The Mean ◽  
K Giants

Abstract We explore the contribution of the Gaia Sausage to the stellar halo of the Milky Way by making use of a Gaussian mixture model (GMM) and applying it to halo star samples of Large Sky Area Multi-Object Fiber Spectroscopic Telescope K giants, Sloan Extension for Galactic Understanding and Exploration K giants, and Sloan Digital Sky Survey blue horizontal branch stars. The GMM divides the stellar halo into two parts, of which one represents a more metal-rich and highly radially biased component associated with an ancient, head-on collision referred to as the Gaia Sausage, and the other one is a more metal-poor and isotropic halo. A symmetric bimodal Gaussian is used to describe the distribution of spherical velocity of the Gaia Sausage, and we find that the mean absolute radial velocity of the two lobes decreases with the Galactocentric radius. We find that the Gaia Sausage contributes about 41%–74% of the inner (Galactocentric radius r gc < 30 kpc) stellar halo. The fraction of stars of the Gaia Sausage starts to decline beyond r gc ∼ 25–30 kpc, and the outer halo is found to be significantly less influenced by the Gaia Sausage than the inner halo. After the removal of halo substructures found by integrals of motion, the contribution of the Gaia Sausage falls slightly within r gc ∼ 25 kpc but is still as high as 30%–63%. Finally, we select several possible Sausage-related substructures consisting of stars on highly eccentric orbits. The GMM/Sausage component agrees well with the selected substructure stars in their chemodynamical properties, which increases our confidence in the reliability of the GMM fits.

Characterisation of V-type asteroids orbiting in the middle and outer main belt

2021 ◽  
Author(s):  
Alessandra Migliorini ◽  
M C De Sanctis ◽  
T A Michtchenko ◽  
D Lazzaro ◽  
M Barbieri ◽  
...  
Keyword(s):  
Near Infrared ◽  
Moving Objects ◽  
Outer Part ◽  
Parent Body ◽  
Sloan Digital Sky Survey ◽  
Asteroid Belt ◽  
Main Belt ◽  
Fe Content ◽  
Principal Finding ◽  
Taxonomical Classification

Abstract We present new spectral observations using ground-based telescopes of 23 putative V-type asteroids, selected according to colour surveys in the visible from the Moving Objects Catalogue of the Sloan Digital Sky Survey and near-infrared from the Moving Objects VISTA catalogue. Ten asteroids are orbiting in the middle main belt, while five in the outer part of the main asteroid belt. For the observed asteroids we assign a taxonomical classification and confirm the basaltic nature for sixteen of them. The high-quality spectra in the UV range, obtained with the X-Shooter spectrograph at ESO, allowed the identification of the Fe2 + forbidden transition of pyroxene for ten asteroids. This band is centred at 506.5 nm, and it is diagnostic of the Ca-content in the pyroxene form. We determined a low Fe-content composition for asteroids (2452) Lyot, (5758) Brunini, (7675) Gorizia, (9197) Endo, (22308) 1990 UO4, (36118) 1999 RE135, (66905) 1999 VC160, and (189597) 2000 WG119, and a composition more rich in Fe for asteroids (75661) 2000 AB79 and (93620) 2000 UQ70. We also present a dynamical investigation of V-type asteroids in the middle and outer main belt. The principal finding of these simulations is that the middle and outer V-types are more likely to be associated with some families, which were considered as possibly originated from the break-up of a partially or totally differentiated parent body by diverse studies. This reinforces the hypothesis that the identified V-type in the region were not originated from (4) Vesta and that the number of differentiated objects in the middle and outer main belt must have been much larger than previously assumed.

scholarly journals The Bimodal Color Distribution of Galaxies at Redshift of z=0-0.15 from the Sloan Digital Sky Survey (SDSS)

2019 ◽  
Vol 30 (2) ◽  
pp. 52
Author(s):  
Hareth Saad Mahdi
Keyword(s):  
Photometric Data ◽  
Sloan Digital Sky Survey ◽  
The Other ◽  
Efficient Tool ◽  
Color Distribution ◽  
Star Forming ◽  
Sky Survey ◽  
Blue Galaxies ◽  
Red Galaxies ◽  
Two Peaks

This work aims to use the color distribution of galaxies to differentiate between blue and red galaxies. The photometric data of 300000 galaxies at redshift of z = 0 – 0.15 were collected from the Sloan Digital Sky Survey (SDSS). Three redshift ranges were considered for the purpose of this work: 100000 galaxies at z = 0-0.05, 100000 galaxies at z = 0.05-0.1 and 100000 galaxies at z = 0.1-0.15. The color distributions for all redshift ranges were determined. The results have clearly shown that the color distributions for all redshift ranges are bimodal. One of the two peaks corresponds to the blue galaxies (young and star-forming galaxies), whereas the other peak corresponds to the red galaxies (old and non-star-forming galaxies). Therefore, the color distribution of galaxies can be considered as an efficient tool to distinguish between blue and red galaxies.

scholarly journals Exploring galaxy colour in different environments of the cosmic web with SDSS

2020 ◽  
Vol 498 (4) ◽  
pp. 6069-6082
Author(s):  
Biswajit Pandey ◽  
Suman Sarkar
Keyword(s):  
Local Density ◽  
Stellar Mass ◽  
Sloan Digital Sky Survey ◽  
Local Dimension ◽  
Sky Survey ◽  
The Galaxy ◽  
Colour Distribution ◽  
The Mean ◽  
Red Galaxies

ABSTRACT We analyse a set of volume-limited samples from the Sloan Digital Sky Survey (SDSS) to study the dependence of galaxy colour on different environments of the cosmic web. We measure the local dimension of galaxies to determine the geometry of their embedding environments and find that filaments host a higher fraction of red galaxies than sheets at each luminosity. We repeat the analysis at a fixed density and recover the same trend, which shows that galaxy colours depend on geometry of environments besides local density. At a fixed luminosity, the fraction of red galaxies in filaments and sheets increases with the extent of these environments. This suggests that the bigger structures have a larger baryon reservoir favouring higher accretion and larger stellar mass. We find that the mean colour of the red and blue populations are systematically higher in the environments with smaller local dimension and increases monotonically in all the environments with luminosity. We observe that the bimodal nature of the galaxy colour distribution persists in all environments and all luminosities, which suggests that the transformation from blue to red galaxy can occur in all environments.

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