Lyman Continuum from z=3 Galaxies

Detections of Lyman Continuum from Star-forming Galaxies at Through Subaru/Suprime-Cam Narrow-band Imaging11affiliation: Based on data collected with the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 22affiliation: Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.

I. Iwata33affiliation: Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Honjo, Kamogata, Asakuchi, Okayama 719-0232; , A. K. Inoue44affiliation: College of General Education, Osaka Sangyo University, 3-1-1 Nakagaito, Daito, Okaka 574-8530, Japan; , Y. Matsuda55affiliation: Department of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan 66affiliation: Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588; , H. Furusawa77affiliation: Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720.; , T. Hayashino88affiliation: Research Center for Neutrino Science, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan;, , K. Kousai88affiliation: Research Center for Neutrino Science, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan;, , M. Akiyama77affiliation: Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720.; 99affiliation: Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, Sendai 980-8578, Japan;, , T. Yamada99affiliation: Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, Sendai 980-8578, Japan;, , D. Burgarella1010affiliation: Laboratoire d’Astrophysique de Marseille, UMR 6110, CNRS/Universite de Provence, 38 rue Joliot-Curie, 13388 Marseille Cedex 13, France;, , and J.-M. Deharveng1010affiliation: Laboratoire d’Astrophysique de Marseille, UMR 6110, CNRS/Universite de Provence, 38 rue Joliot-Curie, 13388 Marseille Cedex 13, France;,

Knowing the amount of ionizing photons from young star-forming galaxies is of particular importance to understanding the reionization process. Here we report initial results of Subaru/Suprime-Cam deep imaging observation of the SSA22 proto-cluster region at , using a special narrow-band filter to optimally trace ionizing radiation from galaxies at . The unique wide field-of-view of Suprime-Cam enabled us to search for ionizing photons from 198 galaxies (73 Lyman break galaxies (LBGs) and 125 Ly- emitters (LAEs)) with spectroscopically measured redshifts . We detected ionizing radiation from 7 LBGs, as well as from 10 LAE candidates. Some of the detected galaxies show significant spatial offsets of ionizing radiation from non-ionizing UV emission. For some LBGs the observed non-ionizing UV to Lyman continuum flux density ratios are smaller than values expected from population synthesis models with a standard Salpeter initial mass function (IMF) with moderate dust attenuation (which is suggested from the observed UV slopes), even if we assume very transparent IGM along the sightlines of these objects. This implies an intrinsically bluer spectral energy distribution, e.g, that produced by a top-heavy IMF, for these LBGs. The observed flux desity ratios of non-ionizing UV to ionizing radiation of 7 detected LBGs range from 2.4 to 23.8 and the median is 6.6. The observed flux density ratios of the detected LAEs are even smaller than LBGs, if they are truly at . We find that the median value of the flux density ratio for the deteced LBGs suggest that their escape fractions is likely to be higher than 4%, if the Lyman continuum escape is isotropic. The results imply that some of the LBGs in the proto-cluster at have the escape fraction significantly higher than that of galaxies (in a general field) at studied previously.

Subject headings:
galaxies: evolution — galaxies: high-redshift — cosmology: observations — intergalactic medium — diffuse radiation
slugcomment: version 20090225, identical to the published one

1. Introduction

Ionizing radiation from star-forming galaxies is a likely primary source of cosmic reionization. Although the ratio of the flux density of Lyman continuum escaping from a galaxy to that produced in the galaxy, the so-called escape fraction (), is a key parameter for evaluating the contribution of galaxies to cosmic reionization, it has been poorly constrained due to the fact that Lyman continuum photons are easily absorbed by the intergalactic medium (IGM). Direct observations of Lyman continuum from galaxies at are virtually impossible because of a rapid increase in the number density of Lyman limit systems toward high redshifts (Inoue & Iwata, 2008). Therefore, we must focus on where the IGM optical depth is still about unity on average. Steidel et al. (2001) detected Lyman continuum in a composite spectrum of 29 Lyman break galaxies (LBGs) at . The observed flux density ratio (i.e., without correction for IGM absorption) was . Shapley et al. (2006, hereafter S06) detected Lyman continuum individually from two out of 14 observed LBGs at through a deep long-slit spectroscopy, and derived and for the two LBGs. For an average of 14 objects, . So far the number of galaxies with direct observation of Lyman continuum is too small to reveal properties shared by galaxies with large , or to estimate a typical value of .

In this paper we report the initial results of the observations of Lyman continuum from galaxies at with Subaru/Suprime-Cam (Miyazaki et al., 2002). A narrow-band filter imaging was adopted to search for Lyman continuum, as pioneered by Inoue et al. (2005) for galaxies at . The use of narrow-band imaging instead of slit spectroscopy enables us to examine ionizing radiation from a large number of galaxies simultaneously, as well as to examine emission offsets from rest-frame non-ionizing UV radiation. The target field of the present study is the SSA22 field where the prominent proto-cluster of galaxies at has been discovered (Steidel et al., 1998, 2000; Hayashino et al., 2004, hereafter H04). We adopt a cosmology with the parameters , and km/s/Mpc. All magnitudes are measured in the AB system.

2. Observations and Data Reduction

We have built a special narrow-band filter NB359 with a central wavelength of 359 nm and a FWHM of 15 nm (and % transmittance between 350 nm and 371 nm). This filter is designed to trace Lyman continuum of galaxies at with a contamination from non-ionizing radiation less than 1% for a typical star-forming galaxy. Laboratory measurements have shown that the transmission of the filter is less than 0.01% in the wavelength range of 400 nm–1200 nm. We also confirmed that the central wavelength is stable with rms=0.47 nm at every position on the filter. In Figure 1 we show the transmission curve of the NB359 filter as well as transmission curves of NB479 which was used in the survey for Ly- emitters (LAEs) at (H04), , , band filters and spectra of model star-forming galaxies at , which is used in section 4.3.

The imaging observations using Subaru/Suprime-Cam with the NB359 filter were carried out in 2007 September 10–14 (UT). Three nights were photometric while in the other two nights cloud coverage was relatively high. The seeing condition was good throughout the observing dates, with a FWHM of in NB359 images. The pointing center (, [J2000]) is aligned to the previous Subaru/Suprime-Cam observations of the SSA22 field (Matsuda et al. 2004, hereafter M04; H04). For half of the shots the position angle was switched from 90°to 270°, in order to reduce the effect of chip-to-chip sensitivity variation.

The data reduction was made using SDFRED version 1.2.5 (Yagi et al., 2002; Ouchi et al., 2004). The rejection of frames under poor sky condition led to a selection of 45 frames with 1,800 sec exposures to produce the mosaic image. The FWHM of point sources is 0.″8. The flux calibration was made using measurements of spectroscopic standard stars. The 3 limiting magnitude of the final mosaic image is estimated to be 27.33 AB mag for diameter aperture. Source detection was done using SExtractor (Bertin & Arnouts, 1996) version 2.5.0, using both -band and NB359 images. Galactic extinction has been corrected using the dust map by Schlegel, Finkbeiner & Davis (1998).

3. Results

There are 198 objects with spectroscopically measured redshifts larger than 3.0 in the Suprime-Cam field-of-view (). Ten objects classified as QSOs/AGNs from optical spectra and/or X-ray observation have already been excluded. Among the 198 objects there are 44 LBGs reported in the literature (Steidel et al., 2003, S06), 29 LBGs selected as -dropout galaxies and identified spectroscopically with VLT/VIMOS (Kousai et al., in preparation), and 125 Ly- emitters (LAEs) and Ly- ’blobs’ selected through a narrow-band (NB497) imaging with Subaru/Suprime-Cam (H04, M04) and identified spectroscopically with Subaru/FOCAS and Keck/DEIMOS (Matsuda et al., 2006, Matsuda et al., in preparation).

We detected 16 objects with secure detection () within 1.″2 diameter apertures in NB359; 6 are LBGs and 10 are LAEs. The redshift range of the LBGs is , while for the LAEs it is . In order to eliminate a possibility of spurious detections, we split the frames used to create the final NB359 image into two sets and generated two mosaic images. All 16 objects were detected in both images at level. We also executed a detection test using a negative image in NB359 and found that a probability of spurious detection at level is %. Therefore, we are confident in the reality of source detection in NB359. In Figures 2 and 3 we show postage stamp images of the detected objects. The objects shown in Figure 2 are within fields observerd with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST; Abraham et al., 2007; Geach et al., 2007), and their F814W images are shown in the figure.

In addition, the object SSA22a-C49, detected in Lyman continuum by S06, has 2.95 significance in our image. The measured flux density within the 1.″2 aperture ( Jy) is consistent with that measured with a long-slit spectroscopy by S06 ( Jy). We add this object to the detection list in NB359, bringing the total number of detected objects to 17 (7 LBGs and 10 LAEs). The images of SSA22a-C49 are shown in Figure 2. On the other hand, we could not find any significant signal in NB359 at the position of SSA22a-D3 which is another object detected in Lyman continuum by S06. Since the 3 detection limit within 1.″2 aperture at the position of this object ( Jy) is well below the flux density reported by S06 ( Jy), it is not clear why the object is not visible in our NB359 image. The images of SSA22a-D3 are also presented in Figure 3.

All of the 10 LAEs detected in NB359 show a prominent emission line around 497 nm in their spectra taken with FOCAS and DEIMOS, but continua are not well detected due to their faintness. All but one spectrum of these 10 objects have a resolution high enough to distinguish the doublet if the emission line detected with the NB497 filter is [O ii] 3727 at , and we find no such feature. However, there is still a possibility that they are AGNs at lower redshifts if the emission line is C iv 1549 at , [C iii] at or Mg ii 2798 at , although some of them show a spatially extended emission in the NB497 image. Unfortunately, the wavelength coverage of the spectra obtained so far is too narrow to definitely rule out the low redshift possibility. Follow-up spectroscopy would be required to clarify whether these objects are really LAEs at .

If a faint foreground object lies very close to an object at , they might mimic Lyman continuum in our NB359, and it would be difficult to distinguish it at longer wavelengths if the object at is brighter than the foreground object. Siana et al. (2007) discussed such a possibility of contamination by faint foreground objects in the Lyman continuum survey. Following Siana et al. (2007), we roughly estimate the probability of such a case by assuming a surface density of faint galaxies and their spatial distribution to be uncorrelated with the objects. The apparent magnitudes of galaxies detected in NB359 range from 26.5 mag to 27.5 mag. The surface number density of galaxies in this magnitude range from -band number count by Williams et al. (1996) is mag deg. If we consider that a foreground object within a 1.″0 radius cannot be distinguished in our NB359 image, each object has 2.4% chance of such foreground contamination. Since we have 198 spectroscopic sample galaxies, several objects among the galaxies detected in NB359 may be explained by contamination by such a foreground object. However, it would be difficult to imagine that all 17 detections could be due to foreground contamination.

4. Discussion

4.1. Spatial Offsets of Lyman Continuum for LBGs

As seen in Figures 2 and 3, shapes and positions of the emitting regions in the 17 detected galaxies in NB359 are quite different from those in the -band, especially for LBGs (marked with circles in Figures 2 and 3). The rms of positional offsets between the NB359 and the -band images for foreground objects with similar magnitude range () is . The offsets of 4 LBGs among the 7 LBGs detected in Lyman continuum exceed , and the average offset is 0.″97 (3.8, corresponding to 7.4 kpc at ). Higher resolution of HST/ACS images clearly shows that in each object with positional offset between NB359 and -band images there are substructures in F814W which agree with the positions of the regions detected in NB359. Except for a few possible cases of foreground contaminations (as discussed in section 3), such differences in the shape and the position between the emitting regions of ionizing radiation and those of non-ionizing UV may give us a clue to understand how Lyman continuum escapes from galaxies. For instance, Lyman continuum may escape through a chimney-like structure in the interstellar medium (Razoumov & Sommer-Larsen, 2007), and we may see the emission only from some limited regions. Another possibility is that the spatial distribution of the Lyman continuum sources is different from that of the non-ionizing UV emitting stars. As shown in Figure 2, the higher spatial resolution of HST/ACS reveals that many of the detected galaxies have multiple knotty structures and that the Lyman continuum emission appears to be associated with one of such knots. Note that at the moment with the F814W image we cannot distinguish between superposition of a foreground object and multiple knotty substructures frequently seen in LBGs (e.g., Lowenthal et al., 1997). The position offsets of Lyman continuum from non-ionizing UV peak also imply a possibility that long-slit spectroscopy may miss Lyman continuum.

4.2. Photometry and Colors of the Detected Objects

Because of the various spatial offsets in the Lyman continuum, using a fixed aperture size to measure the flux for all detected sources is not appropriate to examine the flux ratio between the Lyman continuum and non-ionizing UV emission from these systems. In order to obtain total flux in each image we put the apertures with different radii centered at the peak of an object in -band, examined the curves of growth in NB359 and -band and determined the aperture sizes which are large enough to contain the bulk of fluxes in both images and which do not contain flux from nearby objects. The aperture diameters for the 17 detected galaxies are . In Figure 4 the NB359 colors of the 198 objects with spectroscopic redshifts larger than 3.0 are plotted against their -band magnitudes. The NB359 color corresponds to the apparent flux density ratio of ionizing to non-ionizing UV photons for objects at . For objects detected in the NB359 image, variable aperture sizes described above are used to measure colors, while using arrows we also show colors measured with a aperture, which was used in object detection, both in NB359 and -band. We find that luminous () objects, which roughly correspond to those with of LBGs at (Sawicki & Thompson, 2006), show relatively red colors of NB359. On the other hand, some of the less luminous objects show bluer colors, . If the IGM opacity does not depend on the source luminosity, this suggests that the ionizing-to-non-ionizing UV escape flux density ratio (a proxy of ; see Inoue, Iwata & Deharveng 2006) is lower in relatively luminous objects. Interestingly, this appears contrary to the argument by Gnedin, Kravtsov, & Chen (2008) that is smaller for galaxies with smaller star formation rates (or mass). However, we should note that, as seen in Figure 2, Lyman continuum appear to be emitted from substructures in UV-luminous objects, and the NB359 colors of such substructures would be much bluer than the colors using total flux densities.

4.3. Comparison with Model Stellar Populations

We use deep multi-band optical imaging data (H04) to investigate spectral energy distribution (SED) of the detected sample. The UV spectral slopes of the detected LBGs are flat (). There are two clearly distinctive sub-groups of the detected LAEs from their colors: one is red (), and the other is blue (). In Figure 4 different symbols are used for different types of SEDs. Blue LAEs show extremely blue NB359 colors (), while LBGs have NB359 larger than 0.9. The difference between these three types becomes clear if we place them into the NB359 and two-color plane, as shown in Figure 5. To compare with these observed colors we calculated predictions of colors for young star-forming galaxies with a population synthesis code (Starburst99 version 5.1; Leitherer et al., 1999). A model at zero age, with the Salpeter IMF (0.1–120; Salpeter, 1955) and Padova evolutionary tracks with metallicity is used as a fiducial one. Since models with higher metallicity or older age have redder colors, this model has the bluest SED under an assumption of the Salpeter IMF. The colors of the model without IGM and dust attenuation and assuming at and 3.3 are shown as filled and open circles connected with a solid line in Figure 5. In Figure 5(a) the model does not include flux from nebular continuum and only flux from stellar sources is considered. An arrow indicates the direction of dust attenuation following a prescription by Calzetti et al. (2000) for a galaxy at . For Å we simply extrapolated their attenuation law. Such smooth extrapolation toward extreme-UV may be reasonable up to Å (Draine, 2003). IGM attenuation has a large dispersion for different lines of sight. We show colors with a median value of IGM attenuation for and cases, with the optical depth range containing 68% of all sightlines of Monte-Carlo simulations (Inoue & Iwata, 2008). The shaded area shows colors of model galaxies which can be explained with dust and/or IGM attenuation. The dashed line in the area indicates colors with IGM opacity with 1% probability of occurrence (i.e., very rare transparent sight-lines).

The colors of the detected LBGs suggest moderate attenuation by dust, –0.3, consistent with previous studies (e.g., Iwata, Inoue & Burgarella, 2005). However, the NB359 colors of the detected LBGs are difficult to explain with these models. Even if we assume no IGM attenuation, NB359 colors of the three bluest LBGs cannot be explained. One caveat is that the model SEDs considered in Figure 5(a) do not include nebular continuum. The output SEDs by Starburst99 code have nebular continuum emission assuming all stellar ionizing photons are converted to nebular continuum photons. In Figure 5(b) we show colors of the model with both stellar and nebular continua (i.e., the model is not self-consistent in regard to photon budget). The inclusion of nebular continuum makes SEDs redder in both NB359 and , and in this case the colors of the four redder LBGs would be explained with moderate IGM attenuation. However, there are still three LBGs whose colors cannot be explained with the bluest SED and Calzetti’s dust attenuation law. A QSO-like spectrum may be able to explain these colors. The power-law slope of QSO UV spectrum have large variation. Here we assume two-component power law () with a break at 1100Å, as it is made in the appendix of Inoue & Iwata (2008), and consider the possible bluest color of a QSO at . The power law index at can be as steep as (Scott et al., 2004). At the steepest slope would be (Shang et al., 2005). In such a case NB359 and are and , respectively, without IGM attenuation. Thus by considering IGM attenuation such QSO-like spectrum would be able to explain the colors of the LBGs shown in Figure 5, although these objects are not classified as AGNs, according to the catalog (Steidel et al., 2003).

To explain these strong emission in Lyman continuum without considering possibility of QSOs, models which can produce much bluer intrinsic colors – such as those with a top-heavy IMF – would be required. Indeed, model SEDs with a top-heavy IMF with a slope 1.0 (much steeper than the slope of the Salpeter IMF, 2.35) have mag bluer color in NB359. We also examined colors of the SEDs with zero metallicity stellar population (Population III) with the Salpeter IMF (mass range from 1 to 100) by Schaerer (2003). In Figure 5(a) and (b) the colors of the model at without and with nebular continuum are plotted, respectively. If no nebular continuum is included (Figure 5(a)), the NB359- colors of the Pop-III models are mag bluer than those of Starburst99 models (with Salpeter IMF) and are close to the top-heavy cases.

Alternatively, dust attenuation law might be quite different from that by Calzetti et al. (2000). For example, if the amount of dust attenuation at 900Å is much smaller than that at 1500Å, the dust attenuation arrow approaches vertical in Figure 5, and the NB359 and colors of the LBGs may be explained simultaneously.

Colors of the detected LAEs are much harder to explain with the models considered here. If higher mass cut-off (50–500) is adopted, NB359- color of the Population III model by Schaerer (2003) (using Salpeter IMF and no IGM attenuation is considered) is as small as , and it would be compatible with the bluest LAEs. Thus we would like to stress that, although some of the NB359 colors of the detected objects are unexpectedly blue, such colors are not physically unexplainable and they can be reproduced if we consider metal-poor stellar populations and/or top-heavy IMF. Note that there is a suggestion of the existence of metal-free stellar populations at based on observed data (Jimenez & Haiman, 2006). For a reference, there are three [O ii] emitters at found by the follow-up spectroscopy of the SSA22 LAE survey (Matsuda et al., in preparation). Their colors in NB359 and are 0.90.3 and 0.10.1, respectively, and they are similar to some of LBGs with Lyman continuum detections and are different from those of the detected LAEs. Anyway, deep spectroscopy with wide wavelength coverage is required to confirm their redshifts and explore their nature. In the following discussion for constraints on , we only use the detected LBG sample.

4.4. Constraints on the Escape Fraction

The relative escape fraction is defined as (Steidel et al., 2001):


where and are the intrinsic and observed UV to Lyman continuum flux density ratios, respectively, and is the IGM optical depth for Lyman continuum photons along the line of sight. For the ease of comparison with previous studies on Lyman continuum at (Steidel et al. 2001; Inoue et al. 2005; S06), first we use . If the dust attenuation at 1500 Å  is known, can be converted to as (Inoue et al., 2005; Siana et al., 2007). We calculate the observed flux densities at rest-frame 1500 Å by interpolating flux densities in and -bands, and use flux densities with the NB359 filter as . For different LBGs, different aperture sizes are used to eoncompass the bulk of fluxes and to avoid contamination from neighbours (see section 4.2). For the seven detected LBGs, ranges from 2.4 to 23.8 with a median value of 6.6. If we consider the case without IGM attenuation, this median value corresponds to , and it is a lower limit of (for ). Under the assumption of dust attenuation , which would be reasonable to explain their colors (see Figure 5), a lower limit of is 0.11. If a correction for the IGM attenuation for a median opacity through the NB359 filter (for ) is applied, . One unevitable obstacle to estimate escape fraction from observed flux density ratios is the uncertainty of the intrinsic UV to Lyman continuum flux density ratio which cannot be observed. For the bluest model galaxy generated with Starburst99 (top-heavy IMF, low metallicity, no dust attenuation, no nebular continuum) considered in section 4.3, is 1.07. If we adopt this intrinsic flux ratio instead of 3.0, estimated values of the escape fraction drop. For the case of no IGM attenuation and , is 0.16 and is 0.04. In Table 1 we summarize our estimates of and for LBGs, as well as the average values of obtained by Steidel et al. (2001) and S06. Although there are uncertainties on , amount of dust attenuation and IGM opacity, the high for the LBGs at we obtained makes a clear contrast with a stringent upper limits for stacked images of galaxies (Siana et al., 2007). Also, five among the seven detected LBGs have less than 10. Thus the UV-to-LC ratios of the LBGs detected by us are smaller than the average values of LBGs obtained by Steidel et al. (2001) and S06. However, we should emphasize that, as it is seen in Figure 4, these LBGs should be the systems with smallest among luminous galaxies at . The average of the entire galaxy populations (at least for galaxies) should be much lower than the value derived for our detected LBG sample. The constraints on for UV-magnitude limited sample with the present data will be discussed in a forthcoming paper. Also, we should remind that the SSA22 field is a prominent proto-cluster at , and the properties of ionizing radiation in such an uncommon environment may not be representative of the epoch. A census over a blank field would be required to investigate this point.

We thank Alex Razoumov for a careful read of the manuscript and discussions. We would also like to thank the anonymous referee for helpful comments. II also thanks D. Schaerer for providing the SED data of his Pop-III model, and M. Sawicki and J. P. U. Fynbo for stimulating discussions. II and AKI acknowledge Grant-in-Aid for Young Scientists (B; 18740114) from Japan Society for the Promotion of Science (JSPS) and support by the Institute for Industrial Research, Osaka Sangyo University. We would like to express our acknowledgment to the indigenous Hawaiian community for understanding of the significant role of the summit of Mauna Kea in astronomical research.


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References Sample aa is an assumed intrinsic flux ratio used to derive and from the observed UV to LC flux ratio. has been assumed in the previous studies shown here, and the case corresponds to the bluest model galaxy SED generated with the Starburst 99 code.
Steidel et al. (2001) 29 LBGs, Average 17.73.8 3.0 0.31
Shapley et al. (2006) 2 LBGs, Direct 12.71.8, 7.51.0 3.0 0.43,0.72
Shapley et al. (2006) 14 LBGs, Average 5825 3.0 0.094
This work 7 LBGs, Direct 6.6 (median) 3.0 0.46bbno IGM attenuation is assumed. 0.11cc is assumed.
This work 7 LBGs, Direct 6.6 (median) 3.0 0.83dda median opacity at through the NB359 filter is assumed. 0.20cc is assumed.
This work 7 LBGs, Direct 6.6 (median) 1.07 0.16bbno IGM attenuation is assumed. 0.04cc is assumed.
This work 7 LBGs, Direct 6.6 (median) 1.07 0.30dda median opacity at through the NB359 filter is assumed. 0.07cc is assumed.
Table 1Compilation of observed UV to LC flux ratios and escape fractions of LBGs at .
Figure 1.— Filter transmission curves for the filters used in this study and spectra of a model star-forming galaxy at generated with the Starburst99 code. The solid line represents a model without IGM attenuation, and the dashed line is for a model with average IGM attenuation for objects at . See section 4.3 for details of the model.
Figure 2.— Postage stamp images of objects which are detected in the NB359 image and HST/ACS F814W images are available for them. In each panel NB359 (left), -band (middle) and F814W (right) images are shown. Field of view is 5 5. For the -band and F814W images a contour map of the NB359 image (2 and 3 ) is over-plotted. Symbols at the lower-left of the NB359 images show the object type: filled circles: LBG, filled triangle: ’blue’ LAEs. See section 4.3 for the definition of types. The images of SSA22a-C49, which is one of the two objects repoted to be detected in S06 and is detected in our NB359 image with 2.95 level, is labelled.
Figure 3.— Postage stamp images of objects which are detected in the NB359 image (HST/ACS F814W images are not available). In each panel NB359 (left) and -band (right) images are shown. Field of view is 5 5. For the -band images a contour map of the NB359 image (2 and 3 ) is over-plotted. Here we also show images of SSA22a-D3, which is one of the two objects reported to be detected in Shapley et al. (2006) but is not detected in our NB359 image. Symbols at the lower-left of the NB359 image show the object type: filled circle: LBG, filled triangle: ’blue’ LAEs, and filled squares: ’red’ LAEs. See section 4.3 for the definition of types.
Figure 4.— NB359 colors of objects in the SSA22 field with spectroscopic redshifts . The higher and lower dashed lines indicate approximately and limits in the NB359 image. The objects without significant detection () in the NB359 image are plotted with open circles and upper arrows. The detected LBGs are shown with filled circles. LAEs are classified with two types according to their rest-frame UV slopes: red UV colors (filled squares) and blue UV colors (triangles). See text for details. For the objects detected in the NB359 image, NB359 colors are measured with variable aperture sizes centered at peak positions in -band determined to encompass total fluxes, and arrows indicate how colors change if apertures centered at peaks in NB359 and -band are adopted.

Figure 5.— (a) NB359 and colors of objects detected in NB359. LBGs detected in NB359 are shown with circles, and two LAE sub-groups divided by their UV slopes are shown with open squares and triangles. Filled and open circles connected with a olid line are the color tracks of a model galaxy with the bluest SED with the Salpeter IMF from and 3.3, respectively. The shaded area indicates a color range which can be explained with attenuation by dust and IGM on this model SED. The arrow indicates the direction of dust attenuation following a prescription by Calzetti et al. (2000) and changes in colors with attenuation. Two filled circles with horizontal error bars show the colors of the bluest model SED with the median IGM attenuation at and . The error bars represent the ranges of IGM opacity with 68% probability. The expected colors with the stellar population at zero metallicity based on the SED by Schaerer (2003) from to are also shown (labeled with “Pop-III”). The model galaxy SEDs do not include nebular continuum emission. (b) same as (a) for observed colors of the objects detected in NB359, but model galaxy SEDs include nebular continuum emission.
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