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Richard McMahon, Institute of Astronomy, Cambridge University:…
https://people.ast.cam.ac.uk/~rgm/presentations/26 Jul 2006: Last modified: Wed Jul 26 20:32:26 2006. -
Persistence
https://people.ast.cam.ac.uk/~wfcam/docs/reports/persistence/index.html26 May 2006: The variation measured from faint to bright perturbing star was about 20 counts in the level of the persistent image. ... This indicates that the simple model would only be accurate at the 10-20 counts level. -
https://people.ast.cam.ac.uk/~rgm/vhs/vhs-baseline-v3.txt
https://people.ast.cam.ac.uk/~rgm/vhs/vhs-baseline-v3.txt17 Mar 2006: of 20,000 degree decreases by around 10% for the J/K part. ... 90secs in J/K. UKIDSS LAS Survey ---------------- Median limits(5sigma in 2arcsec aperture) Vega Ks 18.2 H 18.8 J 19.6 Y 20.2. -
CASU WFCAM/VISTA Explanation of documentation numbering system>
https://people.ast.cam.ac.uk/~wfcam/docs_exp.html26 May 2006: scheme.. Dafydd Wyn Evans (dwe @ ast.cam.ac.uk). Last modified: Wed Apr 28 16:20:53 2004. -
Astrometric and Photometric Distortion for WFCAM and VISTA
https://people.ast.cam.ac.uk/~wfcam/docs/reports/astrom/index.html28 Sep 2006: World Coordinate Systems and FITS Headers. After a mere 20 years the FITS community finally agreed upon a standard way of defining a World Coordinate System (WCS) for telescopes with focal -
https://people.ast.cam.ac.uk/~rgm/wfcsur/meetings/announcement_2.txt
https://people.ast.cam.ac.uk/~rgm/wfcsur/meetings/announcement_2.txt5 Dec 2006: products and archive 14:00 Photometric Calibration (Jones/Hodgkin) 14:20 Astrometric Calibration (Bunclark/Lewis/Irwin) 14:40 Pipeline processing I(including demo) (Lewis/Irwin) 15:20 Tea 15:40 Pipeline -
Persistence
https://people.ast.cam.ac.uk/~wfcam/docs/reports/persistence/26 May 2006: The variation measured from faint to bright perturbing star was about 20 counts in the level of the persistent image. ... This indicates that the simple model would only be accurate at the 10-20 counts level. -
Persistence Examples
https://people.ast.cam.ac.uk/~wfcam/docs/reports/persistence/persistence_examples.html26 May 2006: m. 20.3. s. 48 31' 40" and has a 2MASS J magnitude of 8.79. ... The individual frames are 20 second exposures taken in Z. About 20 seconds elapse from the end of 01867 and the start of 01868. -
Astrometric and Photometric Distortion for WFCAM and VISTA
https://people.ast.cam.ac.uk/~wfcam/docs/reports/astrom/28 Sep 2006: World Coordinate Systems and FITS Headers. After a mere 20 years the FITS community finally agreed upon a standard way of defining a World Coordinate System (WCS) for telescopes with focal -
CASU analysis of WFCAM commissioning data - I
https://people.ast.cam.ac.uk/~wfcam/docs/reports/commissioning/index.html2 Nov 2006: The above plots are all in the WFCAM instrumental system and the 5-sigma limiting magnitudes for stellar objects in this data in this system are approximately Y = 20.9, J = ... 20.6, H = 19.8, K = 19.1 ,all in a Vega system. -
Contents
https://people.ast.cam.ac.uk/~wfcam/docs/reports/psf3/17 Jan 2006: A reasonable estimate to account for this is that the 2x2 plots need to be adjusted by 20% (ie. ... However, one of the frames exhibited a large magnitude term in y amounting to 0.05 pixel (20 mas) over the observed magnitude range. -
CASU analysis of SV data for WFCAM
https://people.ast.cam.ac.uk/~wfcam/docs/reports/sv/26 Jan 2006: The images mimic fuzzy looking galaxies and in this image peak at typically 5-20 counts above sky. ... measured using a conventional method) is therefore also 1.20 (Parseval's Theorem and power spectrum <-- FT --> autocorrelation). -
{\bf WFCAM Catalogues}
https://people.ast.cam.ac.uk/~wfcam/docs/catalogues.html4 Feb 2006: 19 Error in pkht. 20 Aperture flux 1 These are a series of different radii soft-edged apertures designed to. ... 26 Aperture flux 4. 27 Error in flux Starting with parameter 20 the radii are:. -
Flat Exposure Properties of VIRCAM Detectors
https://people.ast.cam.ac.uk/~wfcam/docs/reports/vircam_flatreport/8 Dec 2006: 10. VIRCAM_IMG_FLAT255_0049. 15. VIRCAM_IMG_FLAT255_0050. 10. VIRCAM_IMG_FLAT255_0051. 20. VIRCAM_IMG_FLAT255_0052. 10. VIRCAM_IMG_FLAT255_0053. 25. -
WFAU Tapes === Store 6 x dual PCs 3GHz ...
https://people.ast.cam.ac.uk/~wfcam/talks/ukirt_may2006.ppt31 Jul 2006: 2 Tbyte ingest buffer. 10 Tbytes of raw. 20 Tbytes of processed. -
CASU analysis of WFCAM commissioning data - I
https://people.ast.cam.ac.uk/~wfcam/docs/reports/commissioning/2 Nov 2006: The above plots are all in the WFCAM instrumental system and the 5-sigma limiting magnitudes for stellar objects in this data in this system are approximately Y = 20.9, J = ... 20.6, H = 19.8, K = 19.1 ,all in a Vega system. -
Basic Debris Disk Model
https://people.ast.cam.ac.uk/~wyatt/wyat06c.pdf13 Oct 2006: For stars at 2pc SCUBA2 is more sensitive than 70μm at >20-50AU. • -
Dark Exposure Properties of VIRCAM Detectors
https://people.ast.cam.ac.uk/~wfcam/docs/reports/vircam_darkreport/vircam_darkreport.html21 Oct 2006: cosmic rays. Figure 20 A dark corrected dark frame with bad pixels masked out. ... 3. 21.2. 3.9. 4. 24.3. 4.2. 5. 22.7. 4.2. 6. 20.4. -
Estimate of the Number of CPU Nodes to Execute ...
https://people.ast.cam.ac.uk/~wfcam/ukreview/vircam_cpu_estimate.pdf29 Sep 2006: increase the data processing time by approximately 10 to 20%. ... The detailed processing time of this test is:. recipe time = 320 seconds ( 20% for missing functionalities). -
Flat Exposure Properties of VIRCAM Detectors
https://people.ast.cam.ac.uk/~wfcam/docs/reports/vircam_flatreport/vircam_flatreport.html8 Dec 2006: 10. VIRCAM_IMG_FLAT255_0049. 15. VIRCAM_IMG_FLAT255_0050. 10. VIRCAM_IMG_FLAT255_0051. 20. VIRCAM_IMG_FLAT255_0052. 10. VIRCAM_IMG_FLAT255_0053. 25. -
Basic Debris Disk Model
https://people.ast.cam.ac.uk/~wyatt/wyatt_tpf_jul04.ppt19 Apr 2006: They used this result to explain the inner hole in the Pictoris disk by a planet at 20 AU:. ... 850 m : 320 m – 20 cm. Since the size cut-off for resonance is 300 m – 2 mm, I predict:. -
mnr9848.tex
https://people.ast.cam.ac.uk/~wyatt/gfw05.pdf19 Apr 2006: than 20 per cent for stars with twice the metal content of theSun (Fischer & Valenti 2005; Santos et al. ... HD 13445 (K1V) 0.20 HD 10700 (G8V) 0.36HD 143761 (G0V) 0.14 HD 196378 (F7V) 0.32HD 192263 (K2V) 0.07 HD 20794 (G8V) 0.23HD 117176 (G5V) -
LOCAL HEATING IN THE GALACTIC CENTER WESTERN ARC N. ...
https://people.ast.cam.ac.uk/~wyatt/mtpf03.pdf19 Apr 2006: Large-scale mapping of the central 5 pc of the Galaxy at10, 20, and 30 lm at 400 angular resolution by Telesco et al.(1996) found a temperature gradient consistent with ... We estimate a uni-form ISM across our 11.7 and 18.2 lm passbands of 2.86and 2.20, -
, EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des…
https://people.ast.cam.ac.uk/~rgm/vhs/eso-p79b-vhs.pdf5 Oct 2006: whole southern celestial hemisphere (20,000deg2) to a depth 4 magnitudes fainterthan 2MASS/DENIS in at least two wavebands J and K. -
L187 The Astrophysical Journal, 619:L187–L190, 2005 February 1� 2005. …
https://people.ast.cam.ac.uk/~wyatt/ghwd05.pdf19 Apr 2006: Dominik,5 and H. J. Walker6. Received 2004 September 17; accepted 2004 December 20; published 2005 January 10. ... The total dust flux within a diameter circle is′1 37.0mJy at 850mm and mJy at 450mm, in good2.5 250 20. -
L141 The Astrophysical Journal, 532:L141–L144, 2000 April 1q 2000. ...
https://people.ast.cam.ac.uk/~wyatt/ftpk00.pdf19 Apr 2006: The diameter of theP.A. = 1757 5 107major axis of the emission at 10.8 mm is 20.2, which corre-sponds to 215 AU. ... At 18.2 mm the maximum extent of theemission is 20.0 (198 AU), which is about 90% the size ofthe 10 mm emission. -
https://people.ast.cam.ac.uk/~vasily/sdss/456/readme456.txt
https://people.ast.cam.ac.uk/~vasily/sdss/456/readme456.txt27 Jun 2006: The resulting distance moduli are: dmag = [18.2, 20.9, 16.8] In principle, from the CMD matching, you can't really shift the ridgeline by more than 0.05 mag -
Contents
https://people.ast.cam.ac.uk/~wfcam/docs/reports/psf3/index.html17 Jan 2006: A reasonable estimate to account for this is that the 2x2 plots need to be adjusted by 20% (ie. ... However, one of the frames exhibited a large magnitude term in y amounting to 0.05 pixel (20 mas) over the observed magnitude range. -
..............................................................…
https://people.ast.cam.ac.uk/~wyatt/tfwd05.pdf19 Apr 2006: wing along lines through the star. The nine evenly spaced contour levels are at the 10, 20,. ... We ignore results for the regionwithin 20 AU of the star because of the contribution of the silicate feature and uncertaintiesin the PSF. -
CASU analysis of SV data for WFCAM
https://people.ast.cam.ac.uk/~wfcam/docs/reports/sv/index.html26 Jan 2006: The images mimic fuzzy looking galaxies and in this image peak at typically 5-20 counts above sky. ... measured using a conventional method) is therefore also 1.20 (Parseval's Theorem and power spectrum <-- FT --> autocorrelation). -
SUBMILLIMETER OBSERVATIONS OF AN ASYMMETRIC DUST DISK AROUND…
https://people.ast.cam.ac.uk/~wyatt/hgdw03.pdf19 Apr 2006: Received 2002 April 17; accepted 2002 September 20. ABSTRACT. New submillimeter images of the cold dust emission around the nearby main-sequence star Fomalhaut arepresented. ... mJy beam1). Integrated Fluxb. (mJy). 450. 7.1, 12.3 119 20 7.4, 16.2 124 20 -
mnr7957.tex
https://people.ast.cam.ac.uk/~wyatt/gwhd04.pdf19 Apr 2006: Combining this with the beam size, the effectiveresolution is 20 arcsec or 70 au. ... Figure 1. 850-µm image of τ Ceti, smoothed to 20-arcsec resolution. -
Quasars and Galaxies at the Highest Redshifts
https://people.ast.cam.ac.uk/~rgm/presentations/20050922-Crafoord-Symposium.ppt8 Mar 2006: 4400. 22.1. 2.6. V. 5500. 21.3. 3.5. R. 6000. 20.4. 3.9. ... 3000. 22.0. 21.2. 20.0. 19.5. 100. Galactic Plane Magellanic Clouds. 1500. -
Oxford Meeting
https://people.ast.cam.ac.uk/~rgm/presentations/20060412-SKA-Meeting_Oxford.ppt15 Apr 2006: 0.10. V. 5500. 21.3. 21.4. 9.6. 3.5. 0.15. R. 6000. 20.4. ... In some the star–formation at this level may have begun at z10-20. -
PSF Fitting of WFCAM Data: Tests on realdata Document ...
https://people.ast.cam.ac.uk/~wfcam/docs/reports/psf3/psf3.pdf17 Jan 2006: A reasonable estimate to account for this is that the 2x2 plots need to be adjusted by 20% (ie. ... However, one of the frames exhibited a large magnitude term in yamounting to 0.05 pixel (20 mas) over the observed magnitude range. -
Modeling the Structures of Dusty Disks: UnseenPlanets? Mark C. ...
https://people.ast.cam.ac.uk/~wyatt/wyat04a.pdf19 Apr 2006: Consideration of the collisional lifetime of different sizedbodies in the disk showed that what we are seeing is just the bottom half of the cascade(7 µ m dust to 20 ... C., and Taidakova, T. A., Astrophys. J., 537, L147–L151. (2000).20. Macintosh, B. -
��������� ��� ��������������� ��������������…
https://people.ast.cam.ac.uk/~wyatt/wdgj99.pdf19 Apr 2006: 0. 20. 40. Ecl. ipti. c L. atit. ude. 70 80 90 100 110Ecliptic Longitude Relative to Sun. ... 40. -20. 0. 20. 40. 70 80 90 100 110Ecliptic Longitude Relative to Sun. -
Dust_in_the_Debris_Disk_Around_HD69830_09Nov2006
https://people.ast.cam.ac.uk/~wyatt/lbbw07.pdf16 Nov 2006: predominantly Mg-rich olivines (80%) and crystalline pyroxenes (20%) (Figure 3). Unlike our. ... Dark blues - crystalline olivines, forsterite and fayalite, in order of 20 µm amplitude. -
SUBMILLIMETER IMAGES OF A DUSTY KUIPER BELT AROUND � ...
https://people.ast.cam.ac.uk/~wyatt/wgdc05.pdf19 Apr 2006: areconsistent with a ring of radius 150 20 AU seen at 45 25 inclination. ... would migrate from 150to 0 AU (where it would evaporate) on timescales of 20 Myr(Burns et al. -
mnr_7037.tex
https://people.ast.cam.ac.uk/~wyatt/gw03.pdf19 Apr 2006: and Spangler et al. (2000) are also included here – ISO observed 70per cent of the single A stars but only 20 per cent of single G starswithin 25 pc. ... If the r 3 line in Fig. 2 is extrapolatedfrom 20 to 25 pc, the detections should increase to 20 -
PDF/48/aa5873-06.pdf.url
https://people.ast.cam.ac.uk/~wyatt/lwbd06.pdf14 Dec 2006: 2004).These two stars are 10–20 Myr old (see Favata et al. ... 1 AU) while (sub)mm surveys probe cold dust (20 K)distant from the star (100’s AU). -
ESO Public Surveys Proposal Form Phase 1 1 Title: ...
https://people.ast.cam.ac.uk/~rgm/vhs/PS-VHS-v3p0.pdf6 Jun 2006: The proposed VHS survey will have a 10σ limit in Y of 20.4[Vega]; see Table 1. ... UKIDSS LAS uses SDSS z’ with a median 5σ limit(Vega) of 20.3. -
Calibration of WFCAM data from 2MASS: an investiga-tion and ...
https://people.ast.cam.ac.uk/~wfcam/docs/reports/2masscal_old.pdf6 Jan 2006: We analyse photometry of the UKIRT faint standardsmeasured on 20 photometric nights. -
����������� ��� ������������ ������� �!�"���…
https://people.ast.cam.ac.uk/~wyatt/wyat05a.pdf19 Apr 2006: B-! &-. n u= K G %'. Í 20 10 0 -10 -20RA offset, arcsec. ... $9]! ;9:<8 - P7-& (;! (<$ra A ;{' <9];& C#20% '-&- P (--##; 0B#-3 3;,x,- )/5[? -
THE ASTROPHYSICAL JOURNAL, 530 : 329È341, 2000 February 102000. ...
https://people.ast.cam.ac.uk/~wyatt/tfpk00.pdf19 Apr 2006: b) Logarithmic10.8 km levels : 1.3, 1.9, 2.8, 4.2, 6.2, 9.2, 13.7, 20.2, 29.9, 44.3, and 65.5. ... The residual emission (observed minus model ; Fig.4d) at 20 AU from the star is typically 0.2 times that of(0A.3)the lobes. -
arX iv:a stro -ph/ 0504 086 v1 4 A ...
https://people.ast.cam.ac.uk/~wyatt/srms05.pdf19 Apr 2006: from the disk at 160 µm (within the 1-σ contour) is 4Jy 20%. ... At 20 Å, the heating timescale has lengthenedso that larger temperature fluctuations are observed andthe temperature distribution of the grain has a significanthot tail. -
Evolution of Circumstellar Disks Around Normal Stars:Placing Our…
https://people.ast.cam.ac.uk/~wyatt/mbww07.pdf19 Apr 2006: In the two older systems, BD 20 307and HD 69830, this excess is almost entirely silicate emis-sion from small grains. ... statistics suggest a cold debris disk fre-quency of 10–20 % surrounding sun–like stars with a weakdependence on stellar age (Fig. -
arX iv:a stro -ph/ 0311 593 v1 26 N ...
https://people.ast.cam.ac.uk/~wyatt/sdw04.pdf19 Apr 2006: 103 3 20 10 6HD109573 HR4796 A0V 67 0.005 4 8 2 9. ... HD141569 0.0 10.3 2.0 55.0 2.30.5 0.0 20.1 1.9 84 40.9 0.0 99.5 2.4 114 50.5 -
arX iv:a stro -ph/ 0603 608 v2 1 Se ...
https://people.ast.cam.ac.uk/~wfcam/ukreview/dye.pdf28 Sep 2006: 1868 K 3 19.0300 H2 3. Z 1 20.4Y 1 20.3. ... centre with aFWHM of 20′′, and truncated at a maximum offset of 2′. -
Submitted to ApJ 16 July 2006, Accepted 3 October ...
https://people.ast.cam.ac.uk/~wyatt/wsgb07.pdf2 Nov 2006: expect for a belt of a given age, given its radial loca-tion (equations 15-20). ... 3 Substituting in these nominal val-ues into equation (20) and approximating M? =
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