The performance and calibration of WFPC2 on the Huble Space Telescope

Holtzman, Jon A.; Hester, J. J.; Casertano, Stefano; Trauger, John T.; Watson, A. M.; Ballester, G. E.; Burrows, Christopher J.; Clarke, J. T.; Crisp, David; Evans, R. W.; Gallagher, John S.; Griffiths, R. E.; Hoessel, John G.; Matthews, L. D.; Mould, Jeremy; Scowen, Paul A.; Stapelfeldt, K.; Westphal, James A.

doi:10.1086/133533

Cited by 409 publications

(338 citation statements)

References 4 publications

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“…The effect was found to be ≈ 10% at −76 • C and ≈ 4% at −88 • C (Holtzman et al 1995b) in a series of 40 second calibration exposures taken of a field in ω Cen. Elevated sky counts found in longer exposures such as ours are expected to decrease the CTE problem (Holtzman et al 1995a). The lower operating temperature also resulted in far fewer 'hot pixels'; pixels with an elevated dark count lasting for hours or days.…”

Section: Observations and Data Reductionmentioning

confidence: 72%

“…From this procedure we estimated our completeness levels, which are superimposed on Figures 1 and 2. These completeness levels lead to a limiting magnitude ≈ 0.5 magnitudes brighter than initially expected for the refurbished HST, but this is now understood as due to the CCDs leaking some charge between adjacent pixels (Holtzman et al 1995a). These estimates of completeness should be reasonably accurate for the redder stars where hot pixels are not a problem.…”

Section: Completeness Estimatesmentioning

confidence: 79%

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The Metallicity Dependence of the Stellar Luminosity and Initial Mass Function: HST Observations of Open and Globular Clusters

Hippel¹,

Gilmore²,

Tanvir³

et al. 1996

The Astronomical Journal

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Using HST and the WFPC2 we have acquired very deep V-and I-band photometry of stars in NGC 2420 and NGC 2477 to study cluster luminosity functions at approximately solar metallicity. We have determined these cluster luminosity functions down to M I = 10.5 (0.2 M ⊙ ) and find that the luminosity function of NGC 2420 turns over at M I ≈ 9.0, and possibly stops altogether by M I ≈ 9.5. The luminosity function of NGC 2477 may flatten at M I ≥ 9.5. We compare our open cluster luminosity functions to the solar neighborhood field star luminosity function of Kroupa, Tout & Gilmore (1993) Saumon 1995;Alexander et al. 1996). We interpret this smooth and systematic behavior in the cluster luminosity functions as strong evidence in favor of an invariant initial mass function and a metallicity-dependent mass-luminosity relation.

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Section: Observations and Data Reductionmentioning

confidence: 72%

Section: Completeness Estimatesmentioning

confidence: 79%

The Metallicity Dependence of the Stellar Luminosity and Initial Mass Function: HST Observations of Open and Globular Clusters

Hippel¹,

Gilmore²,

Tanvir³

et al. 1996

The Astronomical Journal

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“…The standard reduction steps include bias subtraction, dark current subtraction, and Ñat-Ðelding and are described in detail by Holtzman et al (1995a).…”

Section: Data Reductionmentioning

confidence: 99%

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

Rest

Bosch

Jaffe

et al. 2001

The Astronomical Journal

205

377

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We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 (WFPC2) aboard the Hubble Space T elescope (HST ). This homogeneously selected sample roughly doubles the number of early-type galaxies that have now been imaged at HST resolution and complements similar data on the central regions of radio galaxies and the bulges of spiral galaxies. Our sample strikingly conÐrms the complex morphologies of the central regions of early-type galaxies which have become apparent from previous studies with HST . In particular, we detect dust, either in the form of nuclear disks or with a Ðlamentary distribution, in 43% of all galaxies, in good agreement with previous estimates. In addition, we Ðnd evidence for embedded stellar disks in a remarkably large fraction of 51%. In 14 of those galaxies the disklike structures are misaligned with the main galaxy, suggesting that they correspond to stellar bars in S0 galaxies. We analyze the luminosity proÐles of the galaxies in our sample and classify galaxies according to their central cusp slope. To a large extent we conÐrm the results from previous HST surveys in that early-type galaxies reveal a clear dichotomy : the bright ellipticals are generally boxy and have luminosity proÐles that (M B [ [20.5) break from steep outer power laws to shallow inner cusps (referred to as "" core ÏÏ galaxies). The fainter ellipticals, on the other hand, typically have disky isophotes and luminosity proÐles that lack a clear break and have a steep central cusp (referred to as "" power-law ÏÏ galaxies). The advantages and shortcomings of classiÐcation schemes utilizing the extrapolated central cusp slope c are discussed, and it is shown that c might be an inadequate representation for galaxies whose luminosity proÐle slope changes smoothly with radius rather than resembling a broken power law. Thus, we introduce a new, alternative parameter and show how this a †ects the classiÐcation. In fact, we Ðnd evidence for an "" intermediate ÏÏ class of galaxies that cannot unambiguously be classiÐed as either core or power-law galaxies and that have central cusp slopes and absolute magnitudes intermediate between those of core and power-law galaxies. It is unclear at present, however, whether these galaxies make up a physically distinct class or whether distance and/or resolution e †ects cause them to lose their distinct core or power-law characteristics.

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“…The sample images were first preprocessed through the standard Space Telescope Science Institute (STScI) pipeline, using a standard WFPC2-specific calibration algorithm and the best available calibration files (Holtzman et ale 1995).…”

Section: Sample and Data Reductionmentioning

confidence: 99%

Merging Galaxies with Multiple Nuclei from HST ULIRGs Snapshot Survey

Cui

Xia

Deng

et al. 2001

Symp. - Int. Astron. Union

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Abstract.We perform photometric measurements on a large HST snapshot imaging survey sample of 97 ultraluminous infrared galaxies (ULIRGs). We classify all the sources into three categories with multiple, double and single nucleus/nuclei, mainly based on a quantitative criterion of I-band luminosity. The resultant fractions of multiple, double and single nucleus/nuclei ULIRGs are 18%, 39% and 43%, respectively. This supports the multiple merger scenario as a possible origin of ULIRGs, in addition to the commonly-accepted pair merger model. Further statistical studies indicate that the fraction of AGN increases from multiple (18%) to double (39%) and then to single (43%) nucleus/nuclei ULIRGs. For the single nucleus category, there is a high luminosity tail in the luminosity distribution, which corresponds to a Seyfert l/QSO excess. This supports the statement that active galactic nuclei tend to appear at final merging stage. For multiple and double mergers, we also find a considerably high fraction of very close nucleus pairs (e.g., 2/3 for those separated by less than 5 kpc). This strengthens the conclusion that systems at late merging phase preferentially host ULIRGs.

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The performance and calibration of WFPC2 on the Huble Space Telescope

Cited by 409 publications

References 4 publications

The Metallicity Dependence of the Stellar Luminosity and Initial Mass Function: HST Observations of Open and Globular Clusters

The Metallicity Dependence of the Stellar Luminosity and Initial Mass Function: HST Observations of Open and Globular Clusters

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

Merging Galaxies with Multiple Nuclei from HST ULIRGs Snapshot Survey

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