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Vogeley, Nancy

doi:10.1080/10609169708569914

Cited by 6 publications

(5 citation statements)

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“…We computed the predicted Ñux levels in these bands from our models, and these are plotted in Figure 12 with the same symbols as the near-IR bands. The predicted levels are in good agreement with the Bernstein (1998) and Vogeley (1997) measurements if the redshift of galaxy formation is high ; the numbers for models would produced too much Ñux in these z f \ 3 bands, especially if the Hubble constant is high. It is worth pointing out that because of the Lyman break at 912 in A the spectrum of galaxies, the di †use extragalactic background in the visible bands does not probe as early epochs as those reÑected in the CIB.…”

Section: Near-ir Cosmic Infrared Background Fromsupporting

confidence: 75%

“…Such measurements were provided recently by Bernstein (1998) for the mean (DC) level analysis and by Vogeley (1997) from the Ñuctuations analysis of the Hubble Deep Field. Both give Ñuxes between 10 and 20 nW m~2 sr~1 in B (0.44 m) and R (0.81m) bands ; the results from Bernstein (1998) are plotted as Ðlled circles with error bars.…”

Section: Near-ir Cosmic Infrared Background Frommentioning

confidence: 99%

“…On the other hand, comparable levels can be reached with Ñuctua-tions analysis of the near-IR CIB (Kashlinsky, Mather, & Odenwald 1996 ;Kashlinsky et al 1996 ;Kashlinsky, Mather & Odenwald 1998), and there is hope of reaching the CIB levels directly with this method applied to other surveys. In optical bands, Vogeley (1997) has derived strong limits of the di †use background at R and B from the Ñuc-tuations analysis of the Hubble Deep Field.…”

Section: Introductionmentioning

confidence: 99%

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Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Jiménez

Kashlinsky

1999

ApJ

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Accurate synthetic models of stellar populations are constructed and used in evolutionary models of stellar populations in forming galaxies. Following their formation, the late-type galaxies are assumed to follow the Schmidt law for star formation, while early-type galaxies are normalized to the present-day fundamental plane relations assumed to mimic the metallicity variations along their luminosity sequence. The stars in disks of galaxies are distributed with the Scalo IMF and in spheroids with the Salpeter IMF. We show that these assumptions reproduce extremely well the recent observations for the evolution of the rate of star formation with redshift. We then compute predictions of these models for the observational data at early epochs for various cosmological parameters ), and We Ðnd good ) " , H 0 . match to the metallicity data from the damped Lya systems and the evolution of the luminosity density out to z^1. Likewise, our models produce good Ðts for low values of ) to the deep number counts of galaxies in all bands where data are available ; this is done without assuming existence of extra populations of galaxies at high z. Our models also match the data on the redshift distribution of galaxy counts in B and K bands. They also provide good Ðts to the observed colors. We compute the predicted mean levels and angular distribution of the cosmic infrared background produced from the early evolution of galaxies. The predicted Ñuxes and Ñuctuations are still below the current observational limits, but not by a large factor. Finally, we Ðnd that the recent detection of the di †use extragalactic light in the visible bands requires for our models a high redshift of galaxy formation, otherwise, the proz f º (3È4) ; duced Ñux of the extragalactic light at optical bands exceeds the current observational limits.

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Section: Near-ir Cosmic Infrared Background Fromsupporting

confidence: 75%

Section: Near-ir Cosmic Infrared Background Frommentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Jiménez

Kashlinsky

1999

ApJ

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“…The undetected low-surface-brightness UV-emitting regions should contribute to the total diffuse background in the image. Bernstein (1997) has attempted to measure the mean level of the extragalactic background light (EBL) in the HDF images, while Vogeley (1997) has analyzed the autocorrelation function of the residual fluctuations after masking the galaxies. Vogeley (1997) concludes that diffuse light clustered similarly to faint galaxies can contribute no more than ∼ 20 % of the mean EBL.…”

Section: Dust and Selection Effectsmentioning

confidence: 99%

“…Bernstein (1997) has attempted to measure the mean level of the extragalactic background light (EBL) in the HDF images, while Vogeley (1997) has analyzed the autocorrelation function of the residual fluctuations after masking the galaxies. Vogeley (1997) concludes that diffuse light clustered similarly to faint galaxies can contribute no more than ∼ 20 % of the mean EBL. In contrast Bernstein (1997), concludes that the total optical EBL is two to three times the integrated flux in published galaxy counts.…”

Section: Dust and Selection Effectsmentioning

confidence: 99%

Hubble Deep Fields

Ferguson¹

The Encyclopedia of Astronomy and Astrophysics

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The Hubble space telescope observations of the northern Hubble deep field, and more recently its counterpart in the south, provide detections and photometry for stars and field galaxies to the faintest levels currently achievable, reaching magnitudes V ∼ 30. Since 1995, the northern Hubble deep field has been the focus of deep surveys at nearly all wavelengths. These observations have revealed many properties of high redshift galaxies, and have contributed to important data on the stellar mass function in the Galactic halo. Part 1: Observations, Measurements, and PhenomenologyThe HDFs were carefully selected to be free of bright stars, radio sources, nearby galaxies, etc., and to have low Galactic extinction. The HDF-S selection criteria included finding a quasi-stellar object (QSO) that would be suitable for studies of absorption lines along the line of sight. Field selection was limited to the "continuous viewing zone" around δ = ±62 • , because these declinations allow HST to observe, at suitable orbit phases, without interference by earth -3occultations. Apart from these criteria, the HDFs are typical high-galactic-latitude fields; the statistics of field galaxies or faint Galactic stars should be free from a priori biases. The HDF-N observations were taken in December 1995 and the HDF-S in October 1998. Both were reduced and released for study within 6 weeks of the observations. Many groups followed suit and made data from follow-up observations publicly available through the world wide web.Details of the HST observations are set out in Williams et al. (1996), for HDF-N and in a series of papers for the southern field (Williams et al. 2000;Ferguson et al. 2000;Gardner et al. 2000;Casertano et al. 2000;Fruchter et al. 2000;Lucas et al. 2000). The HDF-N observations primarily used the WFPC2 camera, whereas the southern observations also took parallel observations with the new instruments installed in 1997: the near-infrared camera and multi-object spectrograph (NICMOS) and the space telescope imaging spectrograph (STIS). The area of sky covered by the observations is small: 5.3 arcmin 2 in the case of WFPC2 and 0.7 arcmin 2 in the case of STIS and NICMOS for HDF-S. The WFPC2 field subtends about 4.6 Mpc at z ∼ 3 (comoving, for Ω M , Ω Λ , Ω tot = 0.3, 0.7, 1.0). This angular size is small relative to scales relevant for large-scale structure.The WFPC2 observing strategy was driven partly by the desire to identify high-redshift galaxies via the Lyman-break technique , and partly by considerations involving scattered light within HST (Williams et al. 1996). The images were taken in four very broad bandpasses (F300W, F450W, F606W, and F814W), spanning wavelengths from 2500 to 9000Å. Although filter bandpasses and zeropoints are well calibrated, 2 no standard photometric system has emerged for the HDF. In this review, we use the notation U 300 , B 450 , V 606 and I 814 to denote magnitudes in the HST passbands on the AB system (Oke 1974). On this system m(AB) = −2.5 log f ν (nJy) + 31.4. Where we drop the subscrip...

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Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds

Schlegel

Finkbeiner

Davis

1998

ApJ

14,221

586

16,549

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We present a full-sky 100 km map that is a reprocessed composite of the COBE/DIRBE and IRAS/ ISSA maps, with the zodiacal foreground and conÐrmed point sources removed. Before using the ISSA maps, we remove the remaining artifacts from the IRAS scan pattern. Using the DIRBE 100 and 240 km data, we have constructed a map of the dust temperature so that the 100 km map may be converted to a map proportional to dust column density. The dust temperature varies from 17 to 21 K, which is modest but does modify the estimate of the dust column by a factor of 5. The result of these manipulations is a map with DIRBE quality calibration and IRAS resolution. A wealth of Ðlamentary detail is apparent on many di †erent scales at all Galactic latitudes. In high-latitude regions, the dust map correlates well with maps of H I emission, but deviations are coherent in the sky and are especially conspicuous in regions of saturation of H I emission toward denser clouds and of formation of in molecular clouds. In contrast, H 2 high-velocity H I clouds are deÐcient in dust emission, as expected.To generate the full-sky dust maps, we must Ðrst remove zodiacal light contamination, as well as a possible cosmic infrared background (CIB). This is done via a regression analysis of the 100 km DIRBE map against the Leiden-Dwingeloo map of H I emission, with corrections for the zodiacal light via a suitable expansion of the DIRBE 25 km Ñux. This procedure removes virtually all traces of the zodiacal foreground. For the 100 km map no signiÐcant CIB is detected. At longer wavelengths, where the zodiacal contamination is weaker, we detect the CIB at surprisingly high Ñux levels of 32^13 nW m~2 sr~1 at 140 km and of 17^4 nW m~2 sr~1 at 240 km (95% conÐdence). This integrated Ñux D2 times that extrapolated from optical galaxies in the Hubble Deep Field.The primary use of these maps is likely to be as a new estimator of Galactic extinction. To calibrate our maps, we assume a standard reddening law and use the colors of elliptical galaxies to measure the reddening per unit Ñux density of 100 km emission. We Ðnd consistent calibration using the B[R color distribution of a sample of the 106 brightest cluster ellipticals, as well as a sample of 384 ellipticals with B[V and Mg line strength measurements. For the latter sample, we use the correlation of intrinsic B[V versus index to tighten the power of the test greatly. We demonstrate that the new maps are Mg 2 twice as accurate as the older Burstein-Heiles reddening estimates in regions of low and moderate reddening. The maps are expected to be signiÐcantly more accurate in regions of high reddening. These dust maps will also be useful for estimating millimeter emission that contaminates cosmic microwave background radiation experiments and for estimating soft X-ray absorption. We describe how to access our maps readily for general use.

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Activities

Cited by 6 publications

References 0 publications

Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Galaxy Evolution, Deep Galaxy Counts, and the Near‐Infrared Cosmic Infrared Background

Hubble Deep Fields

Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds

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