EVOLUTION IN THE CONTINUUM MORPHOLOGICAL PROPERTIES OF Ly-Emitting Galaxies From to 111Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
We present a rest-frame ultraviolet morphological analysis of Lyman Alpha Emitters (LAEs) in the Extended Chandra Deep Field South (ECDF-S) and compare it to a similar sample of LAEs at . Using Hubble Space Telescope (HST) images from the Galaxy Evolution from Morphology and SEDs survey, Great Observatories Origins Deep Survey, and Hubble Ultradeep Field, we measure size and photometric component distributions, where photometric components are defined as distinct clumps of UV-continuum emission. At both redshifts, the majority of LAEs have observed half-light radii kpc, but the median half-light radius rises from kpc at to kpc at . A similar evolution is seen in the sizes of individual rest-UV components, but there is no evidence for evolution in the number of multi-component systems. In the sample, we see clear correlations between the size of an LAE and other physical properties derived from its SED. LAEs are found to be larger for galaxies with higher stellar mass, star formation rate, and dust obscuration, but there is no evidence for a trend between equivalent width and half-light radius at either redshift. The presence of these correlations suggests that a wide range of objects are being selected by LAE surveys at , including a significant fraction of objects for which a massive and moderately extended population of old stars underlies the young starburst giving rise to the Ly emission.
Subject headings:cosmology: observations — galaxies: formation – galaxies: high-redshift – galaxies: structure
|Name||Size||HST CoverageaaCounts the total number of objects covered by at least one of GEMS, GOODS, or HUDF||GEMS||GOODS||HUDF||Reference|
|z͡2EWCompletebbz2EWcomplete is a subsample of z2Guaita||130||108||97||19||6||1|
|z3Ciardullo||62ccCounts only those objects that are not already counted in z3Gronwall||55ccCounts only those objects that are not already counted in z3Gronwall||47ccCounts only those objects that are not already counted in z3Gronwall||12ccCounts only those objects that are not already counted in z3Gronwall||0ccCounts only those objects that are not already counted in z3Gronwall||3|
References. – (1) Guaita et al. 2010; (2) Gronwall et al. 2007; (3) Ciardullo et al. 2011
The majority of galaxies in the local universe lie on the Hubble sequence (Hubble, 1936), a continuum that runs between red, passively-evolving galaxies with a compact spheroidal component and gas-rich, star-forming disks with exponential light profiles. This morphological sequence is seen clearly out to intermediate redshifts () (e.g., Glazebrook et al., 1995; van den Bergh et al., 1996; Griffiths et al., 1996; Brinchmann et al., 1998; Lilly et al., 1998; Simard et al., 1999; van Dokkum et al., 2000; Stanford et al., 2004; Ravindranath et al., 2004), beyond which the majority of galaxies appear clumpy and irregular (e.g., Giavalisco et al., 1996; Lowenthal et al., 1997; Dickinson, 2000; van den Bergh, 2001; Papovich et al., 2005; Conselice et al., 2005; Pirzkal et al., 2007) and are difficult to place into existing classification schemes. At , these galaxies, the majority of which are actively star-forming, have sizes ranging from kpc to kpc, with the largest often exhibiting multiple photometric components (e.g., Bouwens et al., 2004; Ravindranath et al., 2006; Oesch et al., 2009).
One of the best-studied classes of galaxies at high redshift is the Lyman Alpha Emitter (LAE). At , LAEs are widely believed to be actively star-forming, low in both stellar and dark matter mass, and relatively dust-free (e.g., Cowie & Hu, 1998; Venemans et al., 2005; Gawiser et al., 2007). The continuum morphological properties of LAEs vary from object to object, but the majority are compact () and have sizes kpc (Venemans et al., 2005; Pirzkal et al., 2007; Overzier et al., 2008; Taniguchi et al., 2009; Bond et al., 2009; Gronwall et al., 2010). Multi-component or clumpy LAEs make up % of the population and typically have morphologies that are qualitatively similar to other star-forming galaxies at high redshift. The emission-line morphologies of LAEs are difficult to study because of the long exposure times required, but Bond et al. (2010) and Finkelstein et al. (2010) find them to be spatially compact ( kpc) at and , respectively. There may be evidence of an additional extended and diffuse component of Ly emission in LAEs at (Nilsson et al., 2009) and (Finkelstein et al., 2010), but Bond et al. (2010) found no evidence for this component in LAEs at , so the question remains open. Using ground-based imaging, Steidel et al. (2011) found extended Ly emission out to kpc around a stack of LAEs identified by the Lyman break technique, but it is unclear to what extent these highly extended halos contribute to the emission-line morphologies of typical LAEs on kiloparsec scales.
The Multiwavelength Survey by Yale-Chile (MUSYC, Gawiser et al., 2006) has obtained multiwavelength imaging and spectroscopy of degree of sky in four fields, including the Extended Chandra Deep Field-South (ECDF-S). As part of this survey, Guaita et al. (2010) (hereafter, Gu10) used broadband and Å narrow-band imaging of the ECDF-S to identify a large, unbiased sample of LAEs at . The authors found the LAEs in this sample to be weakly clustered, with a bias factor, , that is similar to that expected from the progenitors of present-day galaxies. An analysis of the broadband optical and infrared colors of a “stacked” LAE (Guaita et al., 2011) suggests that their median stellar masses ( M) are similar to those of LAEs (Gawiser et al., 2007), although there is a subset of IRAC-bright objects that is times more massive, on average, and exhibits non-negligible amounts of dust reddening, (Lai et al., 2008; Acquaviva et al., 2011).
In this paper, we study the rest-UV continuum morphologies of the Gu10 sample of LAEs and compare them to those seen in LAEs at (Bond et al., 2009; Gronwall et al., 2010) using the samples of Gronwall et al. (2007) and a new sample from Ciardullo et al. (2011). We use images taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS, Rix et al., 2004), Great Observatories Origins Deep Survey (GOODS, Giavalisco et al., 2004), and Hubble Ultradeep Field survey (HUDF, Beckwith et al., 2006). In what follows, we fit each photometric component separately and give quantitative size measures for both the individual components and the LAE system as a whole.
In § 2 and 3, we summarize the data and describe the analysis techniques used in our comparative study. In § 4, we give the photometric properties of each LAE system and its components and compare our results to those found for LAEs. Finally, in § 5, we discuss the implications of our findings for the physical nature of LAEs as a function of redshift. Throughout this paper, we will assume a concordance cosmology with km s Mpc, , and (Spergel et al., 2007). With these values, physical kpc at and physical kpc at .
We use three LAE samples in our analysis, including the equivalent-width-complete subsample of LAEs identified by Gu10, the flux-limited sample of LAEs of Gronwall et al. (2007, z3Gronwall), and the flux-limited sample of LAEs of Ciardullo et al. (2011, z3Ciardullo), all in the ECDF-S. The V-band cutouts and morphological properties of z3Gronwall are already published in Bond et al. (2009, hereafter B09). All samples are summarized in Table 1 and described below.
The initial sample of LAEs (hereafter, z2Guaita) was selected to have a monochromatic flux of ergs cm s, and rest-frame Ly equivalent width of EW Å. For some analyses, the authors made a further cut on Ly luminosity, erg s, in order to remove a bias in their sample against high-EW objects. We use this “equivalent-width complete” subsample (hereafter, z2EWcomplete) of LAEs for the majority of our morphological analyses. Excluding objects within pixels of the edge of an image and cutouts with clear image defects, there are LAEs in z2EWcomplete that are covered by HST broadband imaging surveys.
The two LAE samples used here were both selected to have monochromatic fluxes, ergs cm s, and rest-frame Ly equivalent widths, EW Å. The z3Ciardullo sample covers the same field as z3Gronwall, but identifies LAEs using a narrow-band filter shifted Å to the red relative to the z3Gronwall filter. There remains some overlap between the two filters, however, so % of the objects identified in z3Ciardullo also appear in z3Gronwall. We find additional LAEs in z3Ciardullo that have HST coverage, complementing the LAEs studied in B09. Note that we also exclude objects in these samples that are within ″ of any X-ray source in the expanded catalogs of Lehmer et al. (2005), Virani et al. (2006), and Luo et al. (2008).
Of the surveys used in our study, the GEMS survey covers the largest area, consisting of arcmin of the ECDF-S and ACS pointings in the F606W (V) and F814W (z) filters. The depth of GEMS is relatively uniform across the field, with a detection limit of for V-band point sources. Survey images were multidrizzled (Koekemoer et al., 2002) to a pixel scale of mas. The cutouts for the LAEs in the and samples are shown in Figures 1 and 2 (see end of article), respectively.
The southern half of the GOODS survey is a subregion of the Extended Chandra Deep Field-South, observing arcmin of sky. The GOODS observations included HST/ACS imaging in the F435W (B), V, F775W (I), and z filters. Although the V imaging depth varies across the GOODS area, a typical detection limit for point sources is . As in GEMS, all images were multidrizzled to a pixel scale of mas. The cutouts for the LAEs in the and samples are shown in Figures 3 and 4 (see end of article), respectively.
The Hubble Ultra-Deep Field (HUDF) reaches a V-band point source depth of and includes HST/ACS imaging in the B, V, I, and z filters. The survey covers arcmin of sky and has a multidrizzled pixel scale of mas. The cutouts for the LAEs in z2EWcomplete are shown in Figure 5 (see end of article).
3.1. Visual classification
We have classified all of the objects in z2Guaita with HST coverage according to their morphology in the V cutouts. The morphological classifications are determined by eye, taking into account an object’s size and appearance, where the classes are chosen to separate objects with unusual physical conditions (e.g., apparent major mergers), as well as possible interlopers or contaminants. The four classes are given below.
LCo - Compact objects. Much like the majority of LAEs at , these objects are compact with little or no evidence for extended substructure.
CEx - Clumpy-extended objects. They appear similar to the most extended high-redshift star-forming galaxies (e.g., clump-clusters, Elmegreen et al., 2009), with emission appearing in disconnected clumps.
DEx - Diffuse-extended objects. These objects are large enough to be at least marginally resolved from the ground, with emission dominated by a diffuse component. If they really are at , they are very massive systems, but many are likely to be contaminants or low-redshift interlopers coincident with a high-redshift LAE.
NoD - Non-detected objects. There is no discernable source in the V cutout.
Examples of the LCo, CEx, and DEx classes are shown in Figure 6. Of the objects in z2Guaita with HST coverage, a strong majority (%) are classified as LCo, with the CEx, DEx, and NoD classes making up %, %, and % of the sample, respectively.
The candidate LAEs are plotted in equivalent width vs. Ly luminosity in Figure 7, where symbol type indicates the visual classification. Gu10 selected LAEs according to their narrow-band magnitude rather than their Ly luminosity, leading to a bias against high-equivalent-width LAEs with . Therefore, the majority of our analyses are performed on the subsample with , also referred to as z2EWcomplete. The use of this subsample is further motivated by the small fraction (%) of objects in the DEx class with , as these objects may be dominated by low-redshift contaminants or interlopers within the selection radius.
3.2. Source extraction and aperture photometry
In B09, we describe in detail a data analysis pipeline optimized for measuring the photometric properties of “clumpy” or irregular star-forming galaxies. We will provide only a brief summary here.
For the z3Ciardullo sample, we followed B09 and extracted pixel () cutouts from the GEMS, GOODS, and HUDF images at the ground-based position of each LAE in our sample. Our final sample includes only those LAEs with full survey coverage in the cutout region. We identified all sources in each cutout using SExtractor (Bertin & Arnouts, 1996) with extraction parameters DETECT_MINAREA and DEBLEND_MINCONT, fitting and subtracting a uniform sky from each cutout. In order to determine the rest-UV centroid of each LAE system, we again run SExtractor on each cutout, now with DETECT_MINAREA, and take the flux-weighted mean position of the resulting detections. We follow the same procedure for the z2EWcomplete sample, with the exception that we extract somewhat larger cutouts, pixel (), to provide full coverage for some of the more extended objects in the z2Guaita sample.
For the z3Ciardullo sample, we follow B09 and select sources within . For z2EWcomplete, in order to account for the difference in the angular diameter distance between and , we set . In Figure 8, we plot the distribution of SExtractor V-band detections as a function of angular distance from the ground-based Ly centroid for the objects in z2EWcomplete. Based on the density of sources outside the selection region, we estimate that at most % and % of all LAEs will have an interloper within in z3Ciardullo and z2EWcomplete, respectively. The actual contamination rate will likely be less than this because the presence of an interloping source within ″ will decrease the apparent equivalent width of the LAE in ground-based imaging and make it less likely to exceed the EW cutoff for the surveys.
Following B09, we define the photometric centroid to be the flux-weighted mean position of the detections within . Aperture photometry and half-light radii are computed within fixed apertures with radius, , using the IRAF routine PHOT and centered on the centroid determined from the SExtractor runs.
3.3. Monte Carlo simulations
The HST/ACS images used in this study contain strong pixel-to-pixel correlations as a result of the drizzling process (Koekemoer et al., 2002), so we estimate the uncertainties on the continuum magnitude and half-light radii using Monte Carlo simulations. We perform a total of simulations for each survey, each time placing a Gaussian profile at a random position on the V-band image. The simulated sources have Gaussian profiles with a dispersion between and pixels (between and ) and their photometric properties are computed within a fixed aperture. We define the scatter on a photometric measurement in terms of median statistics:
where and are the first and third quartiles, respectively. In the limit of a well-sampled Gaussian distribution, this quantity approaches the square root of the variance.
The uncertainty on the fixed-aperture magnitudes can be estimated using the weight images provided with each survey, where the pixel-to-pixel flux uncertainty is given by , with the mean being taken over pixel weight values, , in each aperture. When we analyze the scatter in our simulations, we find a linear relationship between the fractional uncertainty in half-light radius and the fractional uncertainty in flux within the aperture (see Figure 9). For the Gaussian model profiles used in our simulations, a least-squares fit yields,
As shown in the figure, this relationship holds for all of the surveys used here (GEMS, GOODS, and HUDF). Furthermore, Figure 10 demonstrates that the fractional uncertainty in half-light radius is independent of half-light radius over the range typical for LAEs ().
As noted in B09, there is a systematic tendency to overestimate the fixed-aperture half-light radius at very faint magnitudes because of the difficulties associated with measuring the light centroid (the center of the aperture) on a discrete grid. This effect does appear in our half-light radius simulations, but it results in only a % overestimate of for marginally resolved sources with V. The effect is even smaller for objects that are more extended and/or brighter than these limits.
4. Lae Morphology Evolution Between and
Between the GEMS, GOODS, and HUDF surveys, there is HST/ACS coverage for a total of LAEs at and, considering only z2EWcomplete, LAEs at . When an object is covered by multiple surveys, we use the cutout from the deeper survey. We note that there are two objects in z2EWcomplete (G and G) ostensibly covered by the GOODS survey that have obvious defects in the V-band images. Both of these objects also have GEMS coverage, so we instead analyze their defect-free GEMS cutouts.
4.1. UV continuum photometric centroid
|NumberaaIndex||Survey||bbDistance between ACS and ground-based centroids||ccHalf-light radius computed by PHOT (not reported for LAEs without SExtractor detections)|
The UV continuum emission in an LAE’s host galaxy travels directly to us from the young stars, but Ly nebular emission can resonantly scatter to large distances from the original starburst, depending on the distribution of neutral hydrogen surrounding the host galaxy. In this circumstance, we might expect to see an offset between the emission-line centroid, measured in a narrow-band filter from the ground, and the rest-frame UV centroid, measured in the V HST/ACS cutouts.
Using the procedure described in Section 3.2, we compute the V-band centroids of all of the objects with HST coverage. There were five objects, one in z3Ciardullo (C34) and four in z2EWcomplete (G168, G206, G218, and G222), for which a centroid could not be computed because SExtractor did not detect any sources within . A visual inspection of their cutouts reveals no evidence for likely counterparts in C34, G206, or G222, but the remaining two have extended sources just outside . For the computation of fixed-aperture magnitudes and half-light radii, we set the centroids of these objects to their ground-based, narrow-band position (the cutout center).
|NumberaaIndex from table 2 of Ciardullo et al. 2010||Survey||bbPosition of ACS centroid (set to ground-based position when there are no SExtractor detections)||bbPosition of ACS centroid (set to ground-based position when there are no SExtractor detections)||ccDistance between ACS and ground-based centroids||ddHalf-light radius computed by PHOT (not reported for LAEs without SExtractor detections)|
In Figure 11, we plot the distribution of measured offsets between the V-band continuum centroids and ground-based emission-line positions in both the z2EWcomplete catalog and the combined LAE catalog. We fit two-dimensional Gaussians to the distributions of centroid offsets and find and for and , respectively. This amount of scatter is consistent with the expected astrometric uncertaintes in the ground-based narrow-band surveys, so we find no evidence for a physical offset between the emission-line and continuum light distributions at the level ( kpc at ) at either redshift.
4.2. Fixed-aperture photometric properties
The fixed-aperture half-light radius measures the size of the LAE “system;” that is, the size of the combined light distribution within of the rest-UV continuum centroid. If, for example, an LAE originates from a pair of merging galaxies with comparable UV continuum brightness, then this half-light radius would be approximately the distance between the galaxies. We give the fixed-aperture V magnitudes, half-light radii, and centroid offsets (relative to the catalog position) for the objects in z2EWcomplete and z3Ciardullo in Tables 2 and 3, respectively. The corresponding tables for z3Gronwall can be found in B09.
In Figure 12, we plot the distribution of fixed-aperture half-light radii for z2EWcomplete and the combined LAE samples. Where a large fraction of the LAEs are near the resolution limit, the majority LAE systems are resolved, with a tail extending to larger half-light radii. The median half-light radii are kpc and kpc for z2EWcomplete and the combined sample, respectively. Using the Kolmogorov-Smirnov (K-S) test and making the null hypothesis that the two samples are drawn from the same half-light radius distribution, we find a -value of . If we exclude those objects in z2EWcomplete classified as DEx in a visual inspection (and therefore less likely to be high-redshift LAEs, see Section 3.1), we find . Finally, even if we exclude all objects with large half-light radii, requiring kpc, we find .
We note that the V filter is centered on rest-frame wavelengths of Å and Å at and , respectively. Although emission at both wavelengths is dominated by UV radiation from young stars, there may still be a difference in the apparent sizes of LAEs between these two parts of the spectrum. To test for this, we compared the sizes of 18 LAEs in the observed-frame B- and V-band imaging from the GOODS survey. We found the B-band (rest-frame Å) sizes to be % larger on average. This may be due to diffuse Ly emission leaking into the B-band filter, but it is difficult to tell from broadband imaging alone. Regardless, these differences only act to increase the size evolution we measure between and . We therefore conclude that, for LAEs selected with the same rest-frame equivalent width and Ly luminosity cutoffs, the systems at are systematically larger than those at .
|NumberaaIndex from table 2 of Gronwall et al. 2007||ComponentbbComponent number||Survey||ccDistance from ground-based Ly position||ddIsophotal axis ratio computed by SExtractor||eeIsophotal position angle computed by SExtractor||ffHalf-light radius computed by SExtractor||SFR(UV)|
In Figure 13, we show the dependence of fixed-aperture half-light radius on UV continuum magnitude for both z2EWcomplete and the combined samples. To make the comparison more direct, we have added mag to the V-band magnitudes, corresponding to the cosmological dimming that would occur if they were seen at . At both redshifts, there is a great deal of scatter that is largely independent of continuum brightness and much larger than the observational uncertainties (which are at V, see Figure 10). In order to test for a correlation between UV continuum magnitude and half-light radius, we have divided the data into five bins in continuum magnitude, computed the mean half-light radius within each bin, and estimated the uncertainty on this mean using bootstrap simulations. The resulting means and their uncertainties are plotted as large points in Figure 13.
There is no evidence for a correlation between and V at - a constant value of kpc is a good fit at . However, the best-fit constant value to the combined LAE sample, kpc, is a significantly poorer fit to the data () than a model where size decreases logarithmically with continuum flux (). The best-fit two-parameter model to the sample is
It is worth noting that this relationship only deviates significantly from the data at faint continuum magnitudes, V, suggesting that this is where most of the size evolution has occurred between and .
We show a similar plot in Figure 14, which gives the relationship between fixed-aperture half-light radius and rest-frame equivalent width. We find no evidence for a correlation between equivalent width and half-light radius at either redshift. This is in line with what is seen in a sample of Lyman break galaxies at , which exhibits little dependence of the UV morphology on the presence or strength of Ly emission (Pentericci et al., 2010).
4.3. Properties of photometric components
|NumberaaIndex from table 2 of Ciardullo et al. 2010||ComponentbbComponent number||Survey||ccDistance from ground-based Ly position||ddIsophotal axis ratio computed by SExtractor||eeIsophotal position angle computed by SExtractor||ffHalf-light radius computed by SExtractor||SFR(UV)|
In the terminology of this paper, a photometric “component” is any contiguous source within of the ground-based Ly centroid of an LAE, where sources are identified in the V HST images using SExtractor (see Section 3.2). We give the brightness, ellipticity, position angle and observed half-light radius () of each LAE component (as computed by SExtractor) for the z2EWcomplete and z3Ciardullo sample in Tables 4 and 5, respectively. We quote half-light radii as computed by SExtractor rather than in fixed apertures in order to avoid blending effects in multi-component systems.
Photometric components can be galaxies themselves or individual star-forming regions within a larger galaxy – it is difficult to distinguish these two possibilities from morphology alone for very compact objects like LAEs. Furthermore, objects with multiple photometric components can be chance coincidences with low-redshift galaxies. In z2EWcomplete, excluding objects classified as DEx, 19 of 108 objects in the sample have more than one photometric component. This is consistent with the 23 of 171 objects (%) with multiple components at , but it is also consistent with our estimated maximum rate of interlopers (%) in the selection region of the LAEs (based on the density of background sources in the cutouts, see Section 3.2). If the majority of multi-component systems in our LAE samples are contaminated by low-redshift interlopers, the distribution of component separations should be consistent with what we would see when comparing the LAE central components to a population with a random angular distribution. To simulate this, we keep the brightest component in each multi-component system and randomly place another component within the selection circle.
We show the normalized distribution of separations for the multi-component systems in our data and mock multi-component systems in Figure 15. At , the real multi-component systems have a median separation of , while the same statistic is for the mock systems. With the null hypothesis that the two samples are drawn from the same parent distribution, the K-S test yields , suggesting that the majority of the components in the multi-component systems in z3Ciardullo and z3Gronwall are associated with LAEs at . By contrast, we cannot exclude the null hypothesis for z2EWcomplete (), despite a smaller median separation in the observed systems () than in the mock systems (). Although this may mean that the multi-component systems in z2EWcomplete are heavily contaminated by interlopers, this result would also be consistent with an increase in the median separation between components in multi-component LAEs from to .
Another way to discern the nature of the multi-component systems is to compare their component size distribution to that of single-component systems. If low-redshift interlopers are common in the multi-component systems, these components might also have larger half-light radii than the average LAE. We show the component size distributions in single- and multi-component systems in Figure 16. The K-S test reveals no evidence that the single- and multi-component systems are drawn from a different parent distribution at either or (). It is therefore unlikely that the multi-component systems at either redshift are dominated by low-redshift interlopers, unless their size distribution is very similar to that of high-redshift LAEs.
In B09, we showed that the half-light radius measured by SExtractor was systematically underestimated for components detected at S/N. For the shallowest survey used here (GEMS), this corresponds to V, so we construct subsamples of components brighter than this limit (including those in multi-component systems). At , the remaining components have kpc, compared to kpc at . With the null hypothesis that the two samples are drawn from the same parent distribution, the K-S test gives , again consistent with an increase in the size of the typical LAE from to .
4.4. Median morphological properties of LAE subsamples
|Subsampleaa LAE subsamples defined in Guaita et al. 2010||Selection||Number of LAEsbbIncludes only LAEs with HST/ACS coverage||Median SizeccMedian fixed-aperture half-light radius within||Size SpreadddInterquartile range of fixed-aperture half-light radius|
Guaita et al. (2011) selected a series of subsamples from the z2Guaita LAEs, separately dividing the sample by Ly equivalent width, rest-frame UV luminosity, m brightness, and BR color. We present the morphological properties of these subsamples in Table 6. In addition to median half-light radius, we give the interquartile range (Q3-Q1) of the half-light radii. Since measurement errors are subdominant to intrinsic scatter in the LAE sizes (see Section 4.2), the latter quantity will give an indication of the morphological heterogeneity within the subsample. Uncertainties on each quantity are estimated from bootstrap simulations.
For comparison, we also create a set of subsamples at . We use the same Ly equivalent width selection criterion as at , but correct the rest-frame UV luminosity and m brightness selection criteria for the difference in luminosity distance. Finally, for the rest-UV color, we use VR instead of BR, attempting to match the rest-frame wavelengths of the bluer band. The properties of each subsample are shown in Table 7.
We find no significant size difference between the high- and low-equivalent width subsamples at either redshift, consistent with the object-by-object results shown in Figure 14. The UV-bright subsamples are larger in both size and size spread than the UV-faint subsamples at both redshifts, but the difference is greater and more statistically significant at , with . A statistically significant difference only appears when we include all of z2Guaita - when the subsamples are restricted to objects in z2EWcomplete, the half-light radius difference between UV-bright and UV-faint subsamples decreases to .
The other two pairs of subsamples, those selected by m flux and BR color, also show a difference between their median half-light radii at . In general, the subsample with the larger median size has properties consistent with what we would expect from objects with a dusty, older stellar population underlying the recent star formation. The brightness at m, in particular, is an indicator of the total stellar mass of an LAE and will be large when a galaxy has undergone previous bursts of star formation. At , we still see a significant size difference between the red and blue LAEs, but the fraction of red LAEs is smaller (% as compared to % at ), indicating that the dusty objects, although still larger in size at , make up a smaller fraction of the LAE population. We see no significant difference in size between the IRAC-faint and IRAC-bright subsamples at , and the fraction of IRAC-bright objects is again smaller (%, as compared to %).
All of the subsamples exhibit a size spread, as indicated by the interquartile range of the half-light radius distribution, that is considerably larger than that expected from the measurement uncertainties alone. The smallest spread ( kpc) is seen in the UV-faint subsample, but its fractional spread (IQR/med) is comparable to that of the other subsamples. The most noticeable outlier is the IRAC-bright subsample, which exhibits a size spread of kpc, suggesting an unusual amount of heterogeneity in this subsample. A comparable spread is not seen in the IRAC-bright subsample.
The case for evolution in the LAE population between and is becoming quite strong. Nilsson et al. (2009), comparing samples of LAEs at and , claim an increase in the AGN fraction and the UV-to-Ly SFR ratio, as well as a narrower EW distribution at . Analyzing the sample studied in this paper, Gu10 confirmed an increase in UV-to-Ly SFR toward , but found no evidence for an increase in the AGN fraction at . Also using the Gu10 sample, Ciardullo et al. (2011) find a % decrease in the number density for sources with erg s, as well as a decrease in both the scale length of the equivalent width distribution and the characteristic luminosity () of the luminosity function at .
There is also evidence that the LAE population is becoming more heterogeneous with time. Nilsson et al. (2011) found increased variety in the SEDs of LAEs at as compared to higher-redshift samples, with only % of the galaxies being consistent with a single, young population of stars. Furthermore, Gu10 find a bimodality in the BR colors of the UV-bright () objects in their sample at , possibly indicating the presence of a sub-population of LAEs for which a significant quantity of dust is present. The evidence for heterogeneity in the z2Guaita sample was further demonstrated in Guaita et al. (2011), where they looked at the SED properties of a series of subsamples selected using various photometric cuts (see also, Section 4.4). In Figures 17, 18, and 19, we show the relationship between the derived SED properties and the median half-light radii of the z2Guaita subsamples333Note that the plotted points are not all independent, as there is overlap in the subsamples. In all cases, we see a wide range of SED properties, as well as a clear correlation between the LAE size and the properties derived from its SED. LAEs are found to be larger for galaxies with higher stellar mass, higher dust obscuration, and higher star formation rate (averaged over Myr, see Guaita et al., 2011). These results are broadly consistent with the numerical simulations of Shimizu & Umemura (2010), who predict that size, stellar mass, and star formation rate will correlate positively with the mass-weighted age of LAEs.
The apparent heterogeneity of LAEs at z might indicate the presence of a sub-population of LAEs that are more massive and more evolved. Such objects would normally have their Ly emission extinguished by dust, but if the galaxies are accreting a relatively pristine subhalo, the Ly emission may be originating from a dust-free star-forming region sufficiently separated from the parent halo that the line emission could escape (Shimizu & Umemura, 2010). Alternatively, the dust in these objects may be concentrated in dense clumps, with the Ly photons resonantly scattering off of the clump surface and escaping the galaxy (e.g., Neufeld, 1991; Hansen & Oh, 2006; Finkelstein et al., 2009). In the simulations of Shimizu & Umemura (2010), only % of LAEs at are evolved galaxies experiencing delayed accretion of a subhalo onto a parent halo rather than galaxies undergoing their first major burst of star formation. By , however, their models show the majority of LAEs (%) are in the former category. This is qualitatively consistent with the increase in size and the broader range of morphological properties that we see at , as well as the increase in dust reddening seen by Guaita et al. (2011).
|Subsample||Selection||Number of LAEsaaIncludes only LAEs with HST/ACS coverage||Median SizebbMedian fixed-aperture half-light radius within||Size SpreadccInterquartile range of fixed-aperture half-light radius|
More work needs to be done before we can properly quantify the size evolution of LAEs through cosmic time. Optimally, we would like to measure size evolution at and in order to determine whether the evolution seen here constitutes a sudden change in the LAE population or a more gradual evolution with redshift. Taniguchi et al. (2009) studied the sizes of a sample of LAEs, fitting a PSF-convolved model to a stack of 43 LAEs and found a best-fit half-light radius of kpc. This can be roughly compared to the median GALFIT-derived size of LAEs in z3Gronwall, kpc (Gronwall et al., 2010), but with the caveat that Taniguchi et al. (2009) were working with a sample that was considerably brighter in Ly ( erg s, Murayama et al., 2007) and Gronwall et al. (2010) were restricting themselves to individual LAEs with S/N in the HST/ACS V images.
It is possible that LAEs will eventually be found to reflect the approximately size evolution of the overall galaxy population (Ferguson et al., 2004), but there are good reasons to think that this will not be the case. LAEs can appear visible to the observer only so long as the Ly radiation is able to escape the galaxy without being absorbed by dust. As such, they likely exist for only a short time after galaxy-scale star formation has turned on and before enough dust is formed to extinguish the Ly. Simulations suggest that this time period could be shorter than years (e.g., Mori & Umemura, 2006). If so, then LAEs are only a single snapshot in the history of a galaxy’s formation and their size evolution should be much less steep than that of the overall galaxy population. If, on the other hand, Ly emission is able to escape from a large fraction of galaxies with previous generations of stars already in place, they should more closely trace the Ferguson et al. (2004) law. The heterogeneity seen in the present samples suggests that the LAE population contains both types of objects, but more work is needed to elucidate whether this division is an actual bimodality or simply a continuous range of properties. The LAE sample, in particular, may contain up to % contamination from low-redshift galaxies (see Section 3.1) - spectroscopic follow-up is needed to accurately estimate the contamination fraction and isolate the types of objects that contribute to the contamination. Furthermore, analysis of the deep rest-frame optical (observed-NIR) imaging obtained as part of the Wide Field Camera 3 Early Release Science (Windhorst et al., 2010) and the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey would allow us to determine where most of the stellar mass in these objects lies and whether it coincides spatially with the rest-UV emission from the young stars.
- REV (????) ????
- 08 (1) 08. 1
- Acquaviva et al. (2011) Acquaviva, V., Gawiser, E., & Guaita, L. 2011, ArXiv:astro-ph/1101.2215
- Beckwith et al. (2006) Beckwith, S. V. W. et al. 2006, AJ, 132, 1729
- Bertin & Arnouts (1996) Bertin, E. & Arnouts, S. 1996, A&AS, 117, 393
- Bond et al. (2010) Bond, N. A., Feldmeier, J. J., Matković, A., Gronwall, C., Ciardullo, R., & Gawiser, E. 2010, ApJ, 716, L200
- Bond et al. (2009) Bond, N. A., Gawiser, E., Gronwall, C., Ciardullo, R., Altmann, M., & Schawinski, K. 2009, Astrophysical Journal, 705, 639
- Bouwens et al. (2004) Bouwens, R. J., Illingworth, G. D., Blakeslee, J. P., Broadhurst, T. J., & Franx, M. 2004, ApJ, 611, L1
- Brinchmann et al. (1998) Brinchmann, J. et al. 1998, ApJ, 499, 112
- Ciardullo et al. (2011) Ciardullo, R. et al. 2011, submitted to ApJ
- Conselice et al. (2005) Conselice, C. J., Blackburne, J. A., & Papovich, C. 2005, ApJ, 620, 564
- Cowie & Hu (1998) Cowie, L. L. & Hu, E. M. 1998, AJ, 115, 1319
- Dickinson (2000) Dickinson, M. 2000, in Royal Society of London Philosophical Transactions Series A, Vol. 358, Astronomy, physics and chemistry of , 2001–+
- Elmegreen et al. (2009) Elmegreen, D. M., Elmegreen, B. G., Marcus, M. T., Shahinyan, K., Yau, A., & Petersen, M. 2009, ApJ, 701, 306
- Ferguson et al. (2004) Ferguson, H. C. et al. 2004, ApJ, 600, L107
- Finkelstein et al. (2009) Finkelstein, S. L., Cohen, S. H., Malhotra, S., & Rhoads, J. E. 2009, ApJ, 700, 276
- Finkelstein et al. (2010) Finkelstein, S. L. et al. 2010, ArXiv:astro-ph/1008.0634
- Gawiser et al. (2006) Gawiser, E. et al. 2006, ApJS, 162, 1
- Gawiser et al. (2007) —. 2007, ApJ, 671, 278
- Giavalisco et al. (1996) Giavalisco, M., Steidel, C. C., & Macchetto, F. D. 1996, ApJ, 470, 189
- Giavalisco et al. (2004) Giavalisco, M. et al. 2004, ApJ, 600, L93
- Glazebrook et al. (1995) Glazebrook, K., Ellis, R., Santiago, B., & Griffiths, R. 1995, MNRAS, 275, L19
- Griffiths et al. (1996) Griffiths, R. E. et al. 1996, in IAU Symposium, Vol. 168, Examining the Big Bang and Diffuse Background Radiations, ed. M. C. Kafatos & Y. Kondo, 219–+
- Gronwall et al. (2010) Gronwall, C., Bond, N. A., Ciardullo, R., Gawiser, E., Altmann, M., Blanc, G. A., & Feldmeier, J. J. 2010, ArXiv:astro-ph/1005.3006
- Gronwall et al. (2007) Gronwall, C. et al. 2007, ApJ, 667, 79
- Guaita et al. (2010) Guaita, L. et al. 2010, ApJ, 714, 255
- Guaita et al. (2011) —. 2011, ArXiv:astro-ph/1101.3017
- Hansen & Oh (2006) Hansen, M. & Oh, S. P. 2006, MNRAS, 367, 979
- Hubble (1936) Hubble, E. P. 1936, Realm of the Nebulae, ed. E. P. Hubble
- Koekemoer et al. (2002) Koekemoer, A. M., Fruchter, A. S., Hook, R. N., & Hack, W. 2002, in The 2002 HST Calibration Workshop : Hubble after the Installation of the ACS and the NICMOS Cooling System, ed. S. Arribas, A. Koekemoer, & B. Whitmore, 337–+
- Lai et al. (2008) Lai, K. et al. 2008, ApJ, 674, 70
- Lehmer et al. (2005) Lehmer, B. D. et al. 2005, ApJS, 161, 21
- Lilly et al. (1998) Lilly, S. et al. 1998, ApJ, 500, 75
- Lowenthal et al. (1997) Lowenthal, J. D. et al. 1997, ApJ, 481, 673
- Luo et al. (2008) Luo, B. et al. 2008, ApJS, 179, 19
- Mori & Umemura (2006) Mori, M. & Umemura, M. 2006, Nature, 440, 644
- Murayama et al. (2007) Murayama, T. et al. 2007, ApJS, 172, 523
- Neufeld (1991) Neufeld, D. A. 1991, ApJ, 370, L85
- Nilsson et al. (2011) Nilsson, K. K., Östlin, G., Møller, P., Möller-Nilsson, O., Tapken, C., Freudling, W., & Fynbo, J. P. U. 2011, A&A, 529, A9+
- Nilsson et al. (2009) Nilsson, K. K. et al. 2009, A&A, 498, 13
- Oesch et al. (2009) Oesch, P. A. et al. 2009, ApJ, 690, 1350
- Overzier et al. (2008) Overzier, R. A. et al. 2008, ApJ, 673, 143
- Papovich et al. (2005) Papovich, C., Dickinson, M., Giavalisco, M., Conselice, C. J., & Ferguson, H. C. 2005, ApJ, 631, 101
- Pentericci et al. (2010) Pentericci, L., Grazian, A., Scarlata, C., Fontana, A., Castellano, M., Giallongo, E., & Vanzella, E. 2010, A&A, 514, A64+
- Pirzkal et al. (2007) Pirzkal, N., Malhotra, S., Rhoads, J. E., & Xu, C. 2007, ApJ, 667, 49
- Ravindranath et al. (2004) Ravindranath, S. et al. 2004, ApJ, 604, L9
- Ravindranath et al. (2006) —. 2006, ApJ, 652, 963
- Rix et al. (2004) Rix, H.-W. et al. 2004, ApJS, 152, 163
- Shimizu & Umemura (2010) Shimizu, I. & Umemura, M. 2010, MNRAS, 406, 913
- Simard et al. (1999) Simard, L. et al. 1999, ApJ, 519, 563
- Spergel et al. (2007) Spergel, D. N. et al. 2007, ApJS, 170, 377
- Stanford et al. (2004) Stanford, S. A. et al. 2004, AJ, 127, 131
- Steidel et al. (2011) Steidel, C. C., Bogosavljević, M., Shapley, A. E., Kollmeier, J. A., Reddy, N. A., Erb, D. K., & Pettini, M. 2011, arXiv:astro-ph/1101.2204
- Taniguchi et al. (2009) Taniguchi, Y. et al. 2009, ApJ, 701, 915
- van den Bergh (2001) van den Bergh, S. 2001, AJ, 122, 621
- van den Bergh et al. (1996) van den Bergh, S., Abraham, R. G., Ellis, R. S., Tanvir, N. R., Santiago, B. X., & Glazebrook, K. G. 1996, AJ, 112, 359
- van Dokkum et al. (2000) van Dokkum, P. G., Franx, M., Fabricant, D., Illingworth, G. D., & Kelson, D. D. 2000, ApJ, 541, 95
- Venemans et al. (2005) Venemans, B. P. et al. 2005, A&A, 431, 793
- Virani et al. (2006) Virani, S. N., Treister, E., Urry, C. M., & Gawiser, E. 2006, AJ, 131, 2373
- Windhorst et al. (2010) Windhorst, R. A. et al. 2010, arXiv:astro-ph/1005.2776