The View from the Center: Slightly off Target

Kleinmann, Howard H.

doi:10.2307/3585460

Cited by 4 publications

(4 citation statements)

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“…(12) Notes are as follows. (a) Not a QSO in the ‘DR3 Quasar Catalogue’, probably because it does not meet the requirement M i > −22 ( H ○ = 70 km s −1 Mpc −1 , Ω M = 0.3 and Ω Λ = 0.7); (b) classified in this work from the presence of C iii ] and Mg ii emission lines in the SDSS DR3 spectrum; (c) spectrum not published; (d) the source is not included in McMahon et al (2002), therefore the APM calibration was adopted; (e) spectrum not available on the SDSS web site; (f) see ; (g) classified as a galaxy in 2MASS (Kleinmann et al 1994).…”

Section: Tng Optical Spectroscopymentioning

confidence: 99%

A FIRST-APM-SDSS survey for high-redshift radio QSOs

Carballo

González‐Serrano

Montenegro‐Montes

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We selected from VLA-FIRST a sample of 94 objects starlike in SDSSS, and with APM colour O-E>2, i.e. consistent with their being high-z QSOs. 78 candidates were classified spectroscopically from published data (mainly SDSS) or observations reported here. The fractions of QSOs (51/78) and z > 3 QSOs (23/78) are comparable to those found in other photometric searches for high-z QSOs. We confirm that O-E>2 ensures inclusion of all QSOs with 3.7 < z < 4.4. The fraction of broad absorption line (BAL) QSOs for 2 < z < 4.4 is 27+-10 per cent (7/26), and the estimated BAL fraction for radio loud (RL) QSOs is at least as high as for optically selected QSOs (about 13 per cent). The high BAL fraction and the high fraction of LoBALs in our sample are likely due to the red colour selection. The space density of RL QSOs for 3.7 < z < 4.4, MAB (1450 A) < -26.6 and P(1.4 GHz) > 10^25.7 W Hz^(-1) is 1.7+-0.6 Gpc^(-3). Adopting a RL fraction 13.4+-3 per cent, this corresponds to rho = 12.5+-5.6 Gpc^(-3), in good agreement with the SDSS QSO luminosity function in Fan et al. (2001). We note the unusual QSO FIRST 1413+4505 (z=3.11), which shows strong associated Lyalpha absorption and an extreme observed luminosity, L about 2 x 10^(15) solar luminosities.Comment: Accepted for publication in MNRAS; 9 figures and 6 tables; Table 2 is in landscape forma

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Section: Tng Optical Spectroscopymentioning

confidence: 99%

A FIRST-APM-SDSS survey for high-redshift radio QSOs

Carballo

González‐Serrano

Montenegro‐Montes

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…Of course, in the modern era the sky is being digitized directly, bypassing photography altogether. This brings many advantages, not the least of which is the ability to survey faster, deeper and at wavelengths other than the optical – e.g., the Sloan Digital Sky Survey (SDSS) (York et al 2000) and the Two–Micron All‐Sky Survey (2MASS) (Kleinmann et al 1994). However, it must be emphasized that for time‐dependent phenomena (e.g., object position and brightness) photographic sky atlases represent a vast archive of invaluable measurements for billions of objects.…”

Section: Introductionmentioning

confidence: 99%

The SuperCOSMOS Sky Survey - I. Introduction and description

Hambly

MacGillivray

Read

et al. 2001

Monthly Notices of the Royal Astronomical Society

551

548

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In this, the first in a series of three papers concerning the SuperCOSMOS Sky Survey (SSS), we give an introduction and user guide to the survey programme. We briefly describe other wide‐field surveys and compare them with our own. We give examples of the data, and make a comparison of the accuracies of the various image parameters available with those from the other surveys providing similar data; we show that the SSS data base and interface offer advantages over these surveys. Some science applications of the data are also described and some limitations discussed. The series of three papers constitutes a comprehensive description and user guide for the SSS.

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“…Infrared surveys are ideal for discovering large samples of cool dwarfs as they are brightest in the near infrared. The first major modern infrared surveys came with the Deep Near Infrared Survey (DENIS; Epchtein et al 1994) and the two‐Micron All‐Sky Survey (2MASS; Kleinmann et al 1994). DENIS covers the southern sky in I , J and K s down to limits of I = 18.5, J = 16.5 and K s = 14.0 while 2MASS is an all sky survey in J , H and K s down to limits of J = 15.8, H = 15.1 and K s = 14.3.…”

Section: Introductionmentioning

confidence: 99%

The possiblity of detection of ultracool dwarfs with the UKIRT Infrared Deep Sky Survey

Deacon

Hambly

2006

Monthly Notices of the Royal Astronomical Society

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We present predictions for the numbers of ultracool dwarfs in the Galactic disc population that could be detected by the WFCAM/UKIDSS Large Area Survey and Ultra Deep Survey. Simulated samples of objects are created with masses and ages drawn from different mass functions and birthrates. Each object is then given absolute magnitudes in different passbands based on empirically derived bolometric correction versus effective temperature relationships (or model predictions for Y dwarfs). These are then combined with simulated space positions, velocities and photometric errors to yield observables such as apparent magnitudes and proper motions. Such observables are then passed through the survey selection mechanism to yield histograms in colour. This technique also produces predictions for the proper motion histograms for ultracool dwarfs and estimated numbers for the as yet undetected Y dwarfs. Finally, it is shown that these techniques could be used to constrain the ultra‐low‐mass mass function and birthrate of the Galactic disc population.

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The View from the Center: Slightly off Target

Cited by 4 publications

References 0 publications

A FIRST-APM-SDSS survey for high-redshift radio QSOs

A FIRST-APM-SDSS survey for high-redshift radio QSOs

The SuperCOSMOS Sky Survey - I. Introduction and description

The possiblity of detection of ultracool dwarfs with the UKIRT Infrared Deep Sky Survey

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