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Sensitivity

Limiting Magnitudes

The limiting magnitude of bHROS is currently set by the relatively high read noise of the CCD and noise due to excess background within the instrument enclosure (see the scattered light page for more information). The table below lists the magnitude, m(nu) that will give a signal-to-noise of 10 in 3600s in 0.7 arcsec seeing for various grating and detector settings. This estimate includes read noise and noise from the excess light.

 Wavelength (A) Object-only Mode Object/Sky Mode
CCD binning CCD binning
1x 4x - 8x 1x 4x - 8x
4500 14.1 mag 14.6 mag 13.7 mag 14.2 mag
5500 14.8 15.3 14.7 15.3
6500 15 15.6 15 15.6
7500 14.9 15.4 15.1 15.6
9000 14 14.5 14.1 14.6

 

Exposure Times

The bHROS Integration Time Calculator is undergoing development and is not yet available. Until that time, the information below, summarizing the sensitivity of bHROS as a function of wavelength1 can be used to estimate the exposure times needed to reach the desired signal-to-noise (Derived from observations of HR 9087 (29 Psc) on July 23/24 2005). The data in the plots and table below give the number of electrons per spectral pixel from the source target.

Important notes in the calculation of the S/N:

  • Plots
  • Table
  • Details
  • Plots give source e- per spectral pixel in 10,000s for m(nu) = 15.0 source (3.66 mJy). See below for details.
    Object-Only Fiber
    (Fiber L5)

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    Object/Sky Fiber
    (Fiber S8)

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    (Opens in a new window)

    Object/Sky Fiber
    (Fiber S1)

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    (Opens in a new window)

     

     



    Table of source e- per spectral pixel in 10,000s
    For m(nu) = 15.0 mag source (3.66 mJy)
    See below for details

      L5 Object Only Fiber S8 Object/Sky Fiber S1 Object/Sky Fiber
    () Order Source e- Source e- Source e-
    4060 50 362
    4143 49 696 425 448
    4229 48 799 480 511
    4319 47 949 562 610
    4413 46 1004 585 651
    4510 45 1102 632 712
    4656 44 1239 715 793
    4764 43 1343 763 880
    4877 42 1479 835 968
    4996 41 1576 881 1037
    5086 40 1653 1144 1102
    5216 39 1758 1214 1200
    5353 38 1894 1310 1293
    5497 37 2034 1399 1399
    5650 36 2171 1481 1526
    5811 35 2285 1532 1621
    5981 34 2416 1604 1715
    6132 33 2501 1550 1746
    6323 32 2599 1650 1795
    6526 31 2739 1720 1901
    6743 30 2798 1774 1966
    6975 29 2838 1811 2063
    7227 28 2814 1811 2118
    7280 28 2632 1951 2106
    7493 27 2608 1685 1976
    7549 27 2340 1739 1888
    7781 26 2313 1488 1759
    7840 26 2005 1490 1621
    8092 25 1946 1254 1438
    8152 25 1744 1278 1415
    8427 24 1534 961 1203
    8490 24 1459 1001 1168
    8858 23 1055 692 820
    9260 22 810 567 644
    9700 21 450 325 339
    10010 20 176 106 130
    10534 19 17.8 10.9 14.3


    Details

    bHROS observations of HR 9087 were obtained on July 23/24 2005, consisting of 100s exposures centered at 4300A, 4900A, 5500A, 6500A, 7500A, 8500A and 9500A (300s), at airmasses ranging from 1.124 to 1.196. Some settings were centered near the peak of the echelle blaze response, while others were centered nearer to the edges of the echellogram which, together with small variations in the seeing between successive exposures, leads to a small degree of scatter in resulting plots of instrumental response versus wavelength.

    The measured seeing at the time of the observations was 0.69 arcsec FWHM. For these conditions 0.724 of the total flux from HR 9087 is predicted to have been encompassed by the 0.88x0.88 arcsec2 effective area of the large slicer aperture while 0.443 of the stellar flux is predicted to have been encompassed by the 0.57x0.57 arcsec2 effective area of the small (dual) bHROS apertures (S1 and S8).

    Monochromatic m(nu) magnitudes for HR 9087 were taken from Hamuy et al. (1994, 106, 566), who tabulate them for 16A bandpasses at 16A steps, from 3300A to 10404A. The zero-magnitude flux calibration for m(nu) is 3.664x10-20 ergs cm-2 s-1 Hz-1 = 3664 Jy. Magnitudes in the broad-band V (5500A) system have the same zero-magnitude flux calibration in Jy as the m(nu) system but broad-band magnitudes at other wavelengths (e.g. B, R, I) do not. A source with an m(nu) magnitude of 15.00 at 4500A, 6800A and 8980A would correspond to B=15.18; R=14.76 and I=14.60, respectively.

    The measured counts per spectral pixel per second from HR 9087 were extrapolated to predict the expected counts per spectral pixel in 10,000s for an m(nu) = 15.0 target (3.66 mJy) in 0.7 arcsec seeing.

     

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    Last update March 10, 2006; Steven Margheim
    1S/N plots and tables prepared by Mike Barlow (UCL), August 2005