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  2. WFC - Photometric Calibration

    https://people.ast.cam.ac.uk/~mike/casu/WFCsur/photom.html
    18 Jan 2000: B'_ccd = 24.52 - 2.5 log10(counts/s) = B - 0.129 B-V. ... where B'_ccd is the natural CCD filter system and B, B-V are on Landolt's 1992 system.
  3. TOPICS IN ASTROPHYSICS Much astrophysical research is…

    https://people.ast.cam.ac.uk/~wyatt/topics1.pdf
    29 Sep 2023: ive accelerationatb xtimespentatb. -(am/b). (b(v)good if perturbationissmall. So, what is the timescale for a star to acquire a cumulative? ... kick per encounter. AV2V. Nr(v/5V)2N/ rate ofencountersnbzv. ave(am(b).(b(v). :Tz(v/m)2/ (nbzv)= v3/(amn)
  4. PowerPoint Presentation

    https://people.ast.cam.ac.uk/~phewett/SandES2017/Lec2017_02.pdf
    9 Oct 2017: mB = m(B) = B = B all used for B-band magnitude. ... U-B = B-V = V-R = V-I =…= J-K = 0.0.
  5. M. Pettini: Introduction to Cosmology — Lecture 12 PHYSICAL ...

    https://people.ast.cam.ac.uk/~pettini/Intro%20Cosmology/Lecture12.pdf
    13 Nov 2018: The absorptionline is optically thin and Wλ is a sensitive measure of N, irrespectively of thevalue of the Doppler parameter b (b =. 2σ, where σ is the one-dimensional. velocity dispersion ... 2. The flat, or logarithmic, part, where 10 < τ0 < 103
  6. INT WFS Photometric Calibration Technical Note 1.0: Determination of…

    https://people.ast.cam.ac.uk/~xmmssc/xidops/xiddocs/int_wfs_tn_photometric_calibration.html
    24 Dec 2004: Standards (with nearby on-chip 'normal' standard stars) p=priority n=number of stars in field p n U-B B-V V-I U B V R I saturation ... Table 2 Red Standards p n U-B B-V V-I U B V R I saturation limit(sec) recommended t_exp(sec) ---------------------------
  7. 28 Sep 2006: 3 }x%$É-3 , uwv $m#A3. tu )ô$ & u -)B& v 1m-3@B@- / v xv #" v ')B&!@0$Ð)B"%@B!,)B-3 %$Y"%$£|) },A#)ô&3@ ÀÅ t ... vÅv $Ð)B@BA'"%@ v x-3",. )B'$Ð,@BA3E0"%$ v -!1, uwv ') v 1m-0&("%$E0)B ')B %&()B@ v )3x v!
  8. lecture8_debrisdiskapp

    https://people.ast.cam.ac.uk/~wyatt/lecture8_debrisdiskapp.pdf
    17 Feb 2009: Lagrange’s planetary equations daj/dt = 0, dz/dt = iAz, dy/dt = By, where A,B are matrices of Aji,Bji. • ... sight. A B. B. A. Face-on view of the disk. Origin of forced eccentricity.
  9. M. Pettini: Structure and Evolution of Stars — Lecture ...

    https://people.ast.cam.ac.uk/~pettini/Stellar%20Structure%20Evolution/Lecture02.pdf
    10 Oct 2023: Hereare some examples:. Table 2.2 B V colours and effective temperaturesof some nearby stars. ... Conven-tionally, colours are specified in the sense (shorter wavelength)(longerwavelength). Thus we have U B, B V , V R, V K, and so on.
  10. THE ASTROPHYSICAL JOURNAL, 530 : 329È341, 2000 February 102000. ...

    https://people.ast.cam.ac.uk/~wyatt/tfpk00.pdf
    19 Apr 2006: W99 ignore the e†ects of radiation pressure,assuming, in e†ect, that large, dynamically stable dustgrains, with b B 0, orbit HR 4796A ; b is the ratio of theradiation pressure ... As discussed in 6, themid-infraredÈemitting particles, if they are
  11. WFC - Photometric Calibration

    https://people.ast.cam.ac.uk/~mike/casu/WFCsur/photom_old.html
    13 Dec 1999: B'_ccd = 24.51 - 2.5 log10(counts/s) = B - 0.13 B-V. ... where B'_ccd is the natural CCD filter system and B, B-V are on Landolt's 1992 system.

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