INTRODUCTION
A STUDY OF HDF-NORTH
CONCLUSIONS
REFERENCES
Published in "Photometric Redshifts and the Detection of High Redshift Galaxies", ASP Conference Series, Vol. 191, 1999. Edited by Ray Weymann, Lisa Storrie-Lombardi, Marcin Sawicki, and Robert Brunner.
Abstract. The increased incidence of morphologically peculiar galaxies at faint magnitudes in the optical could be attributable either to "morphological k-corrections" (the change in appearance when viewing high-z objects at shorter rest-frame wavelengths), or an increase in the incidence of truly irregular systems with redshift. The deep, high-resolution GTO-NICMOS near-IR imaging of a portion of the northern Hubble Deep Field has been combined with the WFPC2 data and photometric redshift estimates to study the redshift evolution of morphology, comparing galaxy appearance at the same rest-wavelengths (Bunker, Spinrad & Thompson 1999). It appears that morphological k-corrections are only significant in a minority of cases, and that once these are accounted for, evolution is still demanded - galaxies were smaller and more irregular in the past, with some of the peculiarities probably merger-related. This multi-waveband data set also enables a study of the spatially-resolved stellar populations in distant galaxies. A near-infrared analysis of some of the brighter spirals shows more pronounced barred structure than in the optical, indicating that the apparent decline in barred spirals at faint magnitudes in the optical HDF may be due to band-shifting effects at the higher redshifts, rather than intrinsic evolution.
Key Words: galaxies: evolution -- galaxies: fundamental parameters (classification) -- galaxies: interactions -- galaxies: irregular -- galaxies: peculiar -- infrared: galaxies
INTRODUCTION
A STUDY OF HDF-NORTH
CONCLUSIONS
REFERENCES
For a postscript version of the article, click here.
When coupled with distance estimates such as photometric redshifts, the study of morphology has the potential to probe the dynamical state and evolution of galaxies. However, morphological classification is only reliable to redshifts of a few tenths when hampered by ground-based seeing. The deep, high-resolution WFPC2 imaging of the Hubble Deep Field (HDF, Williams et al. 1996) dramatically pushed the study of galaxy morphology to faint magnitudes and high redshifts, revealing that by IAB > 24, the traditional Hubble sequence no longer provides an adequate description of most galaxies (Abraham et al. 1996).
Some of the faint peculiar galaxies are sub-luminous irregulars at
modest redshifts, while others are higher-z. But are they "true
peculiars" - the counterparts to local irregulars? Matters are
complicated by morphological k-corrections: for single
waveband selection, shorter rest wavelengths are sampled in higher-z
galaxies. The rest-UV is dominated by sites of recent star formation,
and it is known that the appearance of local Hubble-sequence galaxies
can be very different in the UV compared to the optical (e.g.,
O'Connell 1997).
This change in apparent morphology, resulting from a dispersion of
stellar populations, is well illustrated by some HDF spirals at moderate
redshift (z 
1)
which undergo a complete metamorphosis from the
observed optical to the near-IR (Fig. 1).
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Figure 1. Spiral galaxies at
z | |
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Figure 2. Stellar population fits
to two spatially resolved areas of the
z |
To address whether the apparent increased incidence of peculiars in the optical at faint magnitudes is attributable to genuine evolution in the fraction of irregular galaxies, or whether it is predominantly due to band-shifting effects, the appearance of galaxies over a variety of redshifts should be compared at the same rest wavelength (Fig. 3).
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Figure 3. A montage of galaxies down to IAB < 26.0 which lie within the GTO-NICMOS Hubble Deep Field, ranked in order of redshift. Each galaxy is displayed in the waveband which most closely matches the rest-frame B-band, from the WFPC2 images (F450W-'B', F606W-'V', F814W-'I') and the NIC3 data (F110W-'J', F160W-'H'). Each box is 2arcsec across. At higher redshifts, the incidence of the familiar Hubble-sequence galaxies declines greatly. The identification numbers come from the catalog of Williams et al. (1996), and the photometric redshifts are taken from Fernández-Soto, Lanzetta & Yahil (1999). Those denoted by 'z(sp)' have spectroscopically-determined redshifts. |
We have analyzed galaxy morphology to faint magnitudes in HDF-North
using the optical & near-IR HST images
(Bunker, Spinrad
& Thompson 1999).
We have studied the GTO-NICMOS data set
(Thompson et
al. 1999),
a 1arcmin2 area of the HDF imaged for 49 orbits with NIC3 in
both F110W
( J-band) and F160W
( H-band). Combined
with the four WFPC2 pass-bands
(Fig. 3), this data set
provides deep, multi-color, high-resolution imaging extending out to
1.6 µm - the rest-optical at z ~ 2. We use the
redshifts of the galaxies to match the rest-wavelengths, determine intrinsic
luminosities, and to fit stellar populations/dust reddening to the
spectral energy distributions. Where available, we use the
spectroscopically-measured redshifts (from Cohen et al. 1996 unless
otherwise noted). Where no published spectroscopic redshift exists, we
adopt the photometric redshift estimate of
Fernández-Soto,
Lanzetta & Yahil (1999).
Comparative Morphology: Down to
IAB 26
(the brightest 100 galaxies in GTO-NICMOS field):
only about 1/6 of galaxies change their appearance
greatly between the WFPC2 and NICMOS images - these have large
morphological k-corrections;
about half of the galaxies retain the same
morphology in all
wavebands (above the redshifted Lyman break) and are "true irregulars";
the remaining third of galaxies are too compact
for changes in
morphology to be ascertained (the NIC3 PSF has a FWHM of
0.25arcsec); for most
cosmologies, the higher-redshift systems are on average more compact.
Spatially-Resolved Stellar Populations: Once we correct for different resolutions of NIC3 and WFPC2 (through "PSF matching"), we can use the spatially-resolved colors to study different stellar populations and/or dust-reddening within a galaxy (see Figs. 2 & 5). Some of the galaxies which have the same appearance at all wavelengths fall outside the traditional Hubble tuning-fork diagram, but instead belong to new morphological groups, such as chain galaxies (Fig. 4; Cowie, Hu & Songaila 1995), tadpoles (van den Bergh et al. 1996) and bow-shock systems (Fig. 4).
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Figure 4. Examples of a bow-shock interacting system (left) and a chain galaxy (right). Note the bow-shock area itself is comparatively blue, implying a young stellar population with star formation presumably triggered by the shock front, whereas the redder (older) core of the galaxy is more prominent in the near-IR. The chain galaxy (the two-component U-drop called "the Hot Dog"; Steidel et al. 1996, Bunker et al. 1998) appears the same at all wavelengths and is blue, implying a relatively homogeneous, young population (a primæval galaxy candidate?). | |
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Figure 5. Spatially-resolved colors of the northern and southern components of the chain galaxy called "the Hot Dog" (HDF4-555.1; Fig. 4). The northern and southern components exhibit subtly different colors, attributable to either different stellar populations or non-uniform dust extinction. Adopting the approach of Abraham (1997), we also plot the evolution in the (V - I) and (J - H) colors with time for a Salpeter IMF and an exponentially-decaying star formation rate, with e-folding times ranging from 0.1Gyr to 1Gyr. At z = 2.8, (J - H) straddles the age-sensitive 4000Å break. |
Barred Spirals: Our data can also address the evolution of galactic bars: it has been claimed that at faint magnitudes, the fraction of barred spirals in the optical HDFs declines rapidly (van den Bergh et al. 1996, Abraham et al. 1999). If this is a truly evolutionary effect, then it has great significance for the physics of disk formation: bars are supported by disk self-gravity, so the implication would be either that at high-z the halo mass dominates that of the disk, or there are significant random motions in the stellar orbits (Ostriker & Peebles 1973).
However, when the spirals are imaged in the near-IR, many are revealed to have bars which are absent in the WFPC2 bands (Fig. 6): the bars have similar colors to the bulges (dominated by older, cooler, redder stars). It appears that morphological k-correction effects for the higher-z spirals cause the apparent decline in optically-selected barred spirals at fainter magnitudes. From the small-number statistics of spirals in the GTO-NICMOS field, there is no significant evolution in the incidence of galactic bars.
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Figure 6. The left panel
shows the only optically-selected barred spiral in HDF-North
(van den Bergh et
al. 1996),
and this seems to be through chance alignment of a swath of young stars
with the approximate axis of the true bar. The
galactic bar in the spiral displayed in the right panel is only
recognizable at infrared-wavelengths - at its redshift of
z | |
Some Hubble tuning-fork galaxies only reveal their true morphology in near-IR. This is particularly so for galaxies with a large dispersion in stellar ages and spatially-distinct stellar populations, such as in spiral galaxies. However, such galaxies which undergo a morphological metamorphosis from the WFPC2 to NIC3 images are rare; most retain the same appearance in all wavebands, or are too compact for the structural parameters to be determined. Once the morphological k-corrections have been accounted for, it appears that the fraction of true irregulars does increase at faint magnitudes/high-z. Finally, the deep near-IR data shows that there is no significant evolution in the incidence of barred spirals with redshift: their apparent scarcity in the optical is a band-shifting effect on the older stellar population of their bars. A more detailed description of this work is given in Bunker, Spinrad & Thompson (1999).
Acknowledgments I wish to thank my collaborators on this program, Hyron Spinrad and Rodger Thompson. We are grateful to Ray Weymann and Lisa Storrie-Lombardi at OCIW for organizing an enjoyable and timely workshop on photometric redshifts, and thank Daniel Stern, Leonidas Moustakas and Mark Dickinson for useful discussions. A.J.B. acknowledges by a NICMOS postdoctoral research fellowship, supported in part by NASA grant NAG5-3043. The observations were obtained with the NASA/ESA Hubble Space Telescope operated by the Space Telescope Science Institute managed by the Association of Universities for Research in Astronomy Inc. under NASA contract NAS5-26555.