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Duration distribution of short GRBs. The solid line is the common BeppoSAX/Batse Sample distribution, the dashed one is the normalized 4B Batse distribution, for comparison. | |
{Top panel:} mass function of the Local Group (LG). The points show the space density of LG members containing , after correcting for incompleteness. The solid line shows the field from Zwaan et al. (1997), scaled vertically so as to fit the points. The dotted line is a with a steep upturn at the low mass end, recen... | |
Illustration of the two surveys strips and the distribution of spheres with radii of 1 Mpc around known galaxies (thin circles) and galaxy groups (thick circles). The grey areas indicate the Zone of Avoidance where $|b|<10^\circ$. The solid horizontal lines show the paths of the Arecibo beam. | |
Simple boxplots illustrating CN bandstrength ranges in RGB and AGB stars of NGC 6752, M13, and M4 are shown. For all of the individual abundance boxes, the horizontal line inside a box indicates the median value of $\delta$S(3839). The vertical boundaries of a box show the interquartile range (the middle 50% of the dat... | |
Boxplots of sodium abundances in M13 (Pilachowski 1996b) and field giant stars (Pilachowski 1996a). The statistical abundance distributions represented by each box's vertical boundaries, etc., are as described in Figure 1. The different boxes illustrate the sodium abundance distributions found for RGB tip stars, lowe... | |
The complete LETGS spectrum of Capella, split into three parts for clarity. Note the difference in x and y scale for the three parts. Indicated in the plot are the triplets discussed in the text and a selection of the Fe lines at longer wavelengths. The hundred strongest lines are listed in Table <ref>. | |
The Oxygen VII triplet in the LETGS -1 order spectrum with the resonance (r), the forbidden (f), and the intercombination (i) line. The measured ratios of these lines (from the fitted curve) are given in the text. | |
{Minimum total mass for self-shielding from an external incident flux with intensity $J_{s,0}$ at the Lyman limit. The curves are for different redshift: from the top to the bottom $z=$8.3, 11.4, 15.4, 18.0, 22.1, 29.6. Circles show the value of $M_H$ (open) and $M_{crit}$ (filled). Radiative feedback works only in the... | |
{Ratio between the mass formed and destroyed by a Pop III object as a function of the SNII explosion redshift (solid lines); values larger than one for the ratio define the epochs where Pop IIIs have a {positive feedback} on galaxy formation. Also shown are the shell (proper) radius at cooling, $R_s$ (dotted), and the ... | |
{Possible evolutionary tracks of objects as determined by the processes and feedbacks discussed in this paper} | |
{ Magnification map for a SCDM model (4'$\times$ 4', corresponding to a NGST field) for a source located at $z=10$. The magnification range is 0.7-50. } | |
Differential number counts for the two cosmological models considered ({thick solid line}: SCDM, {thin solid line}: LCDM) as a function of apparent AB magnitude in $J$,$K$,$L$,$M$ bands. Also shown is the NGST limiting magnitude. {Dashed} curves neglect lensing magnification. | |
{Evolution of the dissociated molecular hydrogen (upper set of lines), ionized atomic hydrogen (middle set) and doubly ionized helium (bottom line) filling factor as a function of redshift for different runs: A (solid line), B (dotted), C (dashed-dotted) and D (dashed). (b) same as (a) for runs: A (solid line), A1 (dot... | |
{Number evolution of different objects in the simulation box for run A.} | |
Panel a: 2-10 keV image of the central part ($32' \times 32'$) of the GIS2 field of view. The raw data have been smoothed with a two-dimensional Gaussian filter with $\sigma = 1'$; contours are at 2.5, 3, 4, 5 and 10 sigma above the background. Panel b: the same contours have been overlaid on the "hard-divided-by-soft"... | |
Panel a: 2-10 keV image of the central part ($32' \times 32'$) of the GIS2 field of view. The raw data have been smoothed with a two-dimensional Gaussian filter with $\sigma = 1'$; contours are at 2.5, 3, 4, 5 and 10 sigma above the background. Panel b: the same contours have been overlaid on the "hard-divided-by-soft"... | |
Residuals of the combined GIS2+GIS3 data set compared with the best fit absorbed power law model. | |
Unfolded spectrum, folded spectrum and the residuals of the combined GIS2+GIS3 data set compared with the best fit model (narrow Gaussian line plus "leaky-absorber" continua). | |
POSS II image of the field centered on AXJ2254+1146. The circle represents the 90% confidence level error box of 2 arcmin radius, while the white cross marks the position of the X-ray centroid when the offset measured for the target of the observation is applied (see table 1). | |
SED of AXJ2254+1146: the filled dots represent the photometric data from radio to optical wavelengths while the solid line represents the $1 - 10$ keV best fit spectral model. The arrow represents the upper limit at 12 $\mu$m. The other lines represent mean SED of Seyfert 2 and of non-AGN Spiral galaxies as indicated i... | |
Optical spectrum of UGC 12237. See section 5 for details. | |
The distribution of galaxies projected on the sky in the IRAS and ORS samples. This is an Aitoff projection in Supergalactic coordinates, with $L = 90^\circ, B = 0^\circ$ (close to the Virgo cluster) in the centre of the map. Galaxies within 2000 km/sec are shown as circled crosses; galaxies between 2000 and 4000 km/se... | |
The distribution of radio source from the 87GB and PMN surveys projected on the sky. This is an Aitoff projection in Equatorial coordinates (from Baleisis et al. 1998). | |
A compilation of density fluctuations on different scales from various observations: a galaxy survey, deep radio surveys, the X-ray Background and Cosmic Microwave Background experiments. The measurements are compared with two popular Cold Dark Matter models (with normalization $\sigma_8=1$ and shape parameters $\Gamma... | |
The high signal-to-noise target-of-opportunity NTT spectra of a bulge G-dwarf (right, Lennon et al. 1996) were made possible by multi-site photometric monitoring by GMAN and an accurate prediction for the time of the caustic crossing (left, Alcock et al. 2000). | |
The high signal-to-noise target-of-opportunity NTT spectra of a bulge G-dwarf (right, Lennon et al. 1996) were made possible by multi-site photometric monitoring by GMAN and an accurate prediction for the time of the caustic crossing (left, Alcock et al. 2000). | |
{Left:} The limb-darkened profiles reconstructed from PLANET light curve data (Albrow et al. 1999b) for MACHO 97-BLG-28 (solid lines) are consistent with stellar atmosphere models (dashed lines) for the K2 giant source star. {Right:} Reconstructed stellar profiles in three passbands (lowest curve at star's center is re... | |
{Left:} The limb-darkened profiles reconstructed from PLANET light curve data (Albrow et al. 1999b) for MACHO 97-BLG-28 (solid lines) are consistent with stellar atmosphere models (dashed lines) for the K2 giant source star. {Right:} Reconstructed stellar profiles in three passbands (lowest curve at star's center is re... | |
The light curve of MACHO 98-SMC-01 (left) combines data from five microlensing teams. Dense sampling by PLANET and EROS over the second peak produced the limb-darkening measurements of Fig. <ref>. Data from MACHO/GMAN, MPS and OGLE near the first peak ruled out the higher $\mu_{\rm LS}$ model of PLANET (right, Albrow e... | |
The light curve of MACHO 98-SMC-01 (left) combines data from five microlensing teams. Dense sampling by PLANET and EROS over the second peak produced the limb-darkening measurements of Fig. <ref>. Data from MACHO/GMAN, MPS and OGLE near the first peak ruled out the higher $\mu_{\rm LS}$ model of PLANET (right, Albrow e... | |
Contours of excess magnification ($\pm$1%, $\pm$5%, bold $= \infty = $caustics) for binary lenses of different mass ratio $q$ and separation $b$. Light curves of background point sources with trajectories crossing these contours will deviate from that of a single lens by the indicated amount. Distances are in $\theta_{... | |
Exclusion diagrams for companions to two different microlenses. {Left:} Companions to MACHO 98-BLG-35 are excluded in the shaded regions (Rhie et al. 2000); the larger the mass ratio, the larger the excluded area on the sky. {Right:} Exclusion contours at various significance levels for OGLE-1998-BUL-14 companions of g... | |
Exclusion diagrams for companions to two different microlenses. {Left:} Companions to MACHO 98-BLG-35 are excluded in the shaded regions (Rhie et al. 2000); the larger the mass ratio, the larger the excluded area on the sky. {Right:} Exclusion contours at various significance levels for OGLE-1998-BUL-14 companions of g... | |
Summary of our current knowledge of abundances at high redshift. Metallicity is on a log scale relative to solar, and $N$(H I) is the column density of neutral hydrogen measured in the forest, damped systems and Lyman break galaxies.
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Comparisons between {Starburst99} (Leitherer {et al.} 1999) population synthesis models with different IMFs (green lines - grey in the black and white version of the figure) and the Keck spectrum of MS 1512-cB58 analysed by Pettini {et al.} (2000b) in the region near the C IV doublet (black histogram). | |
K-band spectrum of the Lyman break galaxy Q0201-C6. The dashed vertical lines indicate the locations of OH emission lines from the night sky; although the lines have been subtracted out the spectrum remains very noisy at these wavelengths. It is thus essential to select LBGs at redshifts which place the nebular lines o... | |
Emission line widths in Lyman break galaxies at $z \simeq 3$ and in local galaxies. The horizontal bar spans the range of widths at 20% peak intensity of [O III] lines in a dozen Lyman break galaxies, while the vertical lines at each end of the bar indicate the range of luminosities sampled (Pettini {et al.} in prepara... | |
(Lack of) redshift evolution in the comoving mass density (left, reproduced from Rao & Turnshek 2000; $H_0 = 65$ km s$^{-1}$ Mpc$^{-1}$, $\Omega = 1$) and metallicity (right, from Pettini {et al.} 1999) of damped systems.
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Metallicity distributions, normalised to unity, of DLAs at $z \simeq 2 - 3$ and of stars belonging to the disk and halo populations in the Milky Way. See Pettini {et al.} (1997) for references to the sources of data and further details.
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Metallicity dependence of the abundances of Si and Mn. Small dots are values in Galactic stars from Edvardsson {et al.} (1993) and Nissen & Schuster (1997) for Si, and from Nissen {et al.} (2000) for Mn. The continuous thin lines in the top panel show the range (upper and lower quartiles) spanned by the compilation of ... | |
C IV column density distribution in Q1422+231 at $\langle z \rangle \simeq 3.15$ (reproduced from Ellison {et al.} 2000); $f$($N$) is the number of C IV systems per column density interval and per unit redshift path. The filled circles are the data grouped into bins of 0.3 in log $N$(C IV) for display purposes. The lin... | |
Distribution of $\log_{10}(\chi^{2}_{ml-out})$ versus $\log_{10}(\Delta)$ for a subset of all light curves. The two lines correspond to the adopted cuts. Stars ($\star$) correspond to the seven candidates selected by our analysis. | |
Expected optical depth ($\times 10^{6}$) up to $7\ \rm{kpc}$ for the different components of the Milky Way as a function of the Galactic longitude at $b= -2.\hskip-2pt \degree 5$ for two values of the bar length parameter ($a$). The 4 directions towards the spiral arms are indicated by vertical arrows whose horizontal ... | |
Expected rate versus event timescale towards $\gsct$. Detection efficiencies $\epsilon(\Delta t)$ are taken into account. | |
Energy spectra in three states of Cyg X-1. | |
X$\gamma$ spectra of GX 339-4 in the hard state from simultaneous observations by {Ginga}-OSSE (upper spectrum: Z98) and RXTE-OSSE (lower spectrum: Zdziarski et al., in preparation). The spectra are fitted by the sum of blackbody, thermal Comptonization, and Compton reflection including an Fe K$\alpha$ line. The last t... | |
Correlation between the strength of Compton reflection and the X-ray spectral index in BH binaries. Larger symbols with error bars and smaller ones without them correspond to observations by RXTE and {Ginga}, respectively. Open circles, triangles, squares, and filled squares correspond to Cyg X-1, GX 339-4, Nova Muscae... | |
The geometry with a central, hot plasma surrounded by a cold disk (ZLS99). The cold disk partly enters the hot plasma down to the radius $d$ which determines the spectral hardness and the amount of reflection, resulting in the correlation shown in the solid curve in Figure 3. | |
Spectra in the BMC model simulated by LT99 (statistical errors are comparable to the scatter of the points). The lower and upper spectra correspond to $\dot m=2$ and 4, respectively. The free-falling electrons were assumed to have $kT=5$ and 20 keV, and the power-law parts of the spectra have $\Gamma\simeq 2.9$ and 2.5... | |
The OSSE spectrum of GRO J1655-40 (crosses) compared to the prediction of the BMC model (thin horizontal lines). | |
The soft-state spectrum of Cyg X-1 from an ASCA-RXTE observation fitted by Comptonization by nonthermal electrons (dominating above the break seen in the short-dashed curve at $\sim 15$ keV) as well as by thermal ones (the short-dashed curve below the break), of disk blackbody photons (long dashes), and Compton reflect... | |
Values of $\Gamma$ and $R$ in the hard state of BH binaries (open circles; same as in Figure 3) and neutron-star binaries (open squares), in Seyfert 1s (crosses) and broad-line radio galaxies (asterisks). Large and small symbols correspond to RXTE and {Ginga} data, respectively. For clarity, error bars are not shown. | |
$(B-V)_0$ vs. $(U-V)_0$ and $(V-K)_0$ for M31 globular clusters (triangles) and Galactic GCs (squares). Lines are population synthesis models of ages 8 Gyr (bluer colors) and 16 Gyr (redder colors): Worthey (solid), BC (dashed), KFF (dotted). | |
Color offsets $\Delta(X-V)$ (data$-$models) for Salpeter IMF. ($\Delta V=0$ is plotted to emphasize that the models are normalized to the data at $V$.) Solid lines: 16 Gyr models, dotted lines: 12 Gyr models, dashed lines: 8 Gyr models. The $-1.5$ and $-0.5$ bins in [Fe/H] are Worthey models; the $-1.63$ and $-0.63$ [F... | |
Color offsets $\Delta(X-V)$ or $\Delta(V-X)$ (data$-$models) for Scalo or Miller-Scalo IMF. Symbols same as Figure <ref>. The $-1.5$ and $-0.5$ bins in [Fe/H] are Worthey models; the $-1.63$ and $-0.63$ [Fe/H] bins are KFF models (which have no $\Delta(J-V),\Delta(H-V)$ since they do not predict these colors). | |
Velocity distribution of 20 galaxies in A3570 | |
ROSAT/HRI image of A901 smoothed with a Gaussian of $\sigma=4\arcsec$. This image is a zoom of the dashed square in Fig. <ref>a. The cluster has a very regular and compact structure. | |
ROSAT/HRI image of A1437 smoothed with a Gaussian of $\sigma=24\arcsec$. The point source in the NE is probably not connected with the cluster. | |
Region around A901. a) X-ray image taken with the ROSAT/HRI. Apart from the extended emission of A901 six point-like sources (A-F) are visible (see also Table <ref>). b) Optical image from the Digitized Sky Survey of the same size as a). The X-ray sources A, C and F could be identified with optical counterparts (see Ta... | |
Region around A901. a) X-ray image taken with the ROSAT/HRI. Apart from the extended emission of A901 six point-like sources (A-F) are visible (see also Table <ref>). b) Optical image from the Digitized Sky Survey of the same size as a). The X-ray sources A, C and F could be identified with optical counterparts (see Ta... | |
Radial profiles of two clusters. Left: A901. The filled circles show the cluster profile with the corresponding fit (full line). The crosses show the profile of the source A. For comparison the on-axis PSF of the ROSAT/HRI normalised to the central bin is shown (dashed line). As the source A is not exactly in the centr... | |
Radial profiles of two clusters. Left: A901. The filled circles show the cluster profile with the corresponding fit (full line). The crosses show the profile of the source A. For comparison the on-axis PSF of the ROSAT/HRI normalised to the central bin is shown (dashed line). As the source A is not exactly in the centr... | |
ROSAT/HRI image of A3570. a) In an image smoothed with a Gaussian of $\sigma=6\arcsec$ distinct sources dominate over the faint cluster emission. The sources A, B, C, and E are point-like while D has a small extent. These sources are listed in Table <ref>. b) After subtraction of the five point sources a strongly smoot... | |
ROSAT/HRI image of A3570. a) In an image smoothed with a Gaussian of $\sigma=6\arcsec$ distinct sources dominate over the faint cluster emission. The sources A, B, C, and E are point-like while D has a small extent. These sources are listed in Table <ref>. b) After subtraction of the five point sources a strongly smoot... | |
Sample Fourier spectra of power density, phase lag, and coherence function. The left panels show the results derived from Observation 3 (following Paper 1), and the right panels the results from Observation 10. Note the difference in the shape of the broad-band phase lag spectrum between the two cases. The dotted lines... | |
Sample Fourier spectra of power density, phase lag, and coherence function. The left panels show the results derived from Observation 3 (following Paper 1), and the right panels the results from Observation 10. Note the difference in the shape of the broad-band phase lag spectrum between the two cases. The dotted lines... | |
Energy dependence of time lag. As for Fig. 1, the results for observations 3 and 10 are shown for illustrative purposes. The dotted lines indicate the frequencies of the QPO and its harmonics. | |
Energy dependence of time lag. As for Fig. 1, the results for observations 3 and 10 are shown for illustrative purposes. The dotted lines indicate the frequencies of the QPO and its harmonics. | |
Evolution of QPO phase lag with X-ray flux. Filled circles show the measured ({soft}) phase lag associated with the fundamental component, while the open circles the lag with the first harmonic. Note that starting at the second period of the rising phase (i.e., Observation 8) both the soft and hard lags increase marked... | |
Evolution of coherence function during the 1998 outburst. The results shown are for the 8.1-13.3 keV band (with respect to the reference band; see main text). They were derived by averaging over 0.004-0.1 Hz, where the coherence function is roughly constant. | |
Energy dependence of coherence function. The results from Observation 3 are shown, as an example. As for Fig. 4, the results are for the 8.1-13.3 keV band and derived by averaging over 0.004-0.1 Hz. | |
The distribution of probabilities, that the observed excess number of events at the candidate TeV position was a background fluctuation, for each of the 54 bursts. The curve indicates the expected distribution of probabilities for a sample drawn from background. The entry at -4.5 corresponds to GRB 970417a. | |
Number of events recorded by Milagrito during T90 in overlapping 1.6$^\circ$ radius bins in the vicinity of GRB 970417a. | |
GRB 970417a: (a) The crosses indicate the arrival time of events from within a 1.6$^\circ$ radius of the candidate TeV counterpart for $\pm$15 s around the start of T90. The histogram shows the same data binned in 1 second intervals. (b) The Milagrito data integrated in 1 sec intervals for $\pm$100 s around the start o... | |
The implied fluence ($>$ 50 GeV) of very high energy emission from GRB 970417a as a function of high-energy cutoff for five assumed differential spectral indices. | |
Properties of the Type I X-ray bursts from EXO 0748-676 from Gottwald et al. (1986). The value of $\alpha$ (top panel) and the apparent black-body radius ($R_{app}$ for $d=10 \ {\rm kpc}$) in the tail of the burst, are shown as a function of the persistent X-ray flux, $F_x=L_x/4\pi d^2$. The solid squares denote those ... | |
A montage showing the Type I burst profile from GS 1826-238 from RXTE as well as the reprocessed optical emission (from Kong et al. 2000). The long duration of the burst is indicative of the delayed energy release from the rapid proton (rp) process. | |
Ratio of extended flux to PSC flux (filled circles) or point-source-filtered addscan flux (open circles), as a function of optical diameter. The open circles are displaced slightly to the right for clarity. The inner error bars are the uncertainty on the ratio, the outer error bars are the population scatter. Where $D_... | |
PSCz versus literature redshifts. Error bars show combined errors. | |
$n(z)$ distribution for high latitude PSCz survey. Error bars are $J_3$-weighted. The line is the prediction from the selection function. | |
Parametric and non-parametric selection functions for high latitude PSCz survey (line and filled circles). Also shown are the QDOT (open circles) and 1.2Jy (crosses) non-parametric selection functions. | |
Source counts for all high latitude sky (filled circles), high latitude 2HCON sky (open circles), and area with potential SAA problems (triangles). | |
Source counts for identified PSCz galaxies as a function of $100 \mum$ background, $I_{100} < 7.5 \MJy\pster$ (filled circles), 7.5-15 (open circles) and 15-22.5 (triangles). | |
15431 PSCz sources identified as possible or definite galaxies, high $|b|$ and default masks in galactic coordinates. | |
Sky distribution of PSCz sources without redshift, with galaxy identifications $b_J<19.5^m$ (open circles, 192 sources) and fainter than this or with no identification (crosses, 542 sources). | |
Left (a) The distribution of spins of NSs in LMXBs, summarizing Tables 1-4 of {<cit.>}. Right (b) Characteristic signal amplitude $h_c$ for several known LMXBs (symbols, see text) compared with the sensitivity $h_{3/{\rm yr}}$ of LIGO-II in broadband (the dotted line) and narrowband (the solid line) configuration (prov... | |
Left (a) The distribution of spins of NSs in LMXBs, summarizing Tables 1-4 of {<cit.>}. Right (b) Characteristic signal amplitude $h_c$ for several known LMXBs (symbols, see text) compared with the sensitivity $h_{3/{\rm yr}}$ of LIGO-II in broadband (the dotted line) and narrowband (the solid line) configuration (prov... | |
Left (a) A cartoon description of how a transverse temperature gradient leads to a varying altitude for the e$^-$ captures. Right (b) The quadrupole $Q_{22}$ due to a single capture layer in the inner crust as a function of $\dot{M}$. The solid and dashed lines denote the results for several NS models for a $10\%$ comp... | |
Left (a) A cartoon description of how a transverse temperature gradient leads to a varying altitude for the e$^-$ captures. Right (b) The quadrupole $Q_{22}$ due to a single capture layer in the inner crust as a function of $\dot{M}$. The solid and dashed lines denote the results for several NS models for a $10\%$ comp... | |
Critical spin frequencies of the r-mode instability. The solid line is the critical frequency set only by shear and bulk viscosities in the core (same as Fig. 1 of B. Owen's review in this volume). The dashed line also includes viscous boundary layer damping, while the shading around it displays the effect of core supe... | |
The field geometry and some closed orbits for the $m=0.01$ case. The upper panel shows the lines of constant $|\vec r\times\grad\phi_c |$ in the $x-z$ plane. The lower panels show the projections of some closed orbits on the $x-z$ and $x-y$ planes. The three symbols $\Box$, $\triangle$, and $\diamond$ show their crossi... | |
The same as Figure 1 with $m=0.04$ for $4$ orbits. | |
The calculated Milky Way warp. Shown are the crossing points of two stable, test-particle orbits for two satellite-to-disk mass ratios: 0.1 (circles), and 0.2 (crosses). The central bar marks one disk scale length (=3 kpc) on each side. The heavy line shows the observed warp of the galaxy. The arrow marks the direction... | |
Schematic view of the Baikal Telescope {NT-200}. The expansion left-hand shows 2 pairs of optical modules ("svjaska") with the svjaska electronics module, which houses parts of the read-out and control electronics. Top right, the 1996 array {NT-96} is sketched. | |
Upper limits to the differential flux of high energy neutrinos obtained by different experiments as well as upper bounds for neutrino fluxes from a number of different models. The triangle denotes the FREJUS limit.
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Fast cooling (FC) synchrotron spectra from a shock injected power law electron distribution. The shape of the spectrum is determined by the ordering of the self absorption frequency, $\nu_{sa}$, with respect to $\nu_c<\nu_m$. There are three possible shapes for the spectrum, corresponding to $\nu_{sa}<\nu_c$, $\nu_c<\n... | |
{Upper Panel} - Histogram of the relativistically-corrected velocity offsets for the 63 confirmed cluster members of CL1604+4304 and CL1604+4321. The offsets are calculated relative to the mean velocity of the supercluster. The solid lines indicate the best-fit Gaussian distribution for each cluster (Postman, Lubin & O... | |
The resulting $(B-R)$ and $(R-i)$ color-magnitude (CM) diagrams from the Palomar imaging of the supercluster region. The small dots represent all galaxies which have been detected in the images. The dashed lines indicate the magnitude limits of the survey. The CM diagrams show a well-defined sequence of red galaxies, m... | |
Histogram of the $(R-i)$ colors of all galaxies with $20 \le i \le 23.5$. The vast majority of galaxies belong to the field population which has an average color of $(R-i) \approx 0.7$. The red sequence of supercluster members is defined by the narrower peak at $(R-I) \approx 1.4$ (indicated by the arrow) and is easily... | |
The same $(R-i)$ color-magnitude diagram as shown in Figure <ref>. The circles indicate all of the spectroscopically-confirmed, early-type galaxies in the two clusters which lie within the field-of-view of our supercluster observations. The color of these galaxies are consistent with the color of the red locus, indicat... |
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