LUMINOUS INFRARED GALAXIES

Figure 1: Integrated spectra of elliptical, spiral, and irregular galaxies, from Kennicutt (1992b). The fluxes have been normalized to unity at 5500 Å.

Figure 2: Relationship between star formation rate (SFR) per unit broadband luminosity in the UBV passbands and integrated color, from the evolutionary synthesis models of Kennicutt et al (1994). The...

Figure 3: Distribution of integrated Hα + [NII] emission-line equivalent widths for a large sample of nearby spiral galaxies, subdivided by Hubble type and bar morphology. The right axis scale shows ...

Figure 4: Distributions of 40- to 120-μm infrared (IR) luminosity for nearby galaxies, normalized to near-IR H-band luminosity, as a function of Hubble type. Adapted from Devereux & Hameed (1997), wi...

Figure 5: Correlation between disk-averaged SFR per unit area and average gas surface density, for 61 normal disk galaxies. Symbols are coded by Hubble type: Sa–Sab (open triangles); Sb–Sbc (open cir...

Figure 6: Relationship between integrated far-infrared (FIR) luminosity and molecular gas mass for bright IR galaxies, from Tinney et al (1990; open circles) and a more luminous sample by Sanders et ...

Figure 7: Correlation between disk-averaged SFR per unit area and average gas surface density, for 36 IR-selected circumnuclear starbursts. See Figure 5 for a similar comparison for normal spiral dis...

Figure 8: A schematic illustration of the evolution of the stellar birthrate for different Hubble types. The left panel shows the evolution of the relative SFR with time, following Sandage (1986). Th...

Figure 9: (Left) The global Schmidt law in galaxies. Solid points denote the normal spirals in Figure 5, squares denote the circumnuclear starbursts in Figure 7. The open circles show the SFRs and ga...

Figure 1: The mean temperature structure of the 3D hydrodynamical model of Trampedach et al. (in preparation) used throughout this review is shown as a function of optical depth at 500 nm (blue solid ...

Figure 2: Comparison of the predicted continuum center-to-limb variation as a function of wavelength for different solar model atmospheres against observations (Neckel & Labs 1994). The results for fi...

Figure 3: The predicted spectral line profile of a typical Fei line from the 3D hydrodynamical solar model (blue solid line) compared to the observations (gray rhombuses). The agreement is clearly ver...

Figure 4: The present-day solar photospheric elemental abundances as a function of atomic number. As throughout this review, the logarithmic abundance of H is defined to be log εH = 12.0.

Figure 5: Comparison of the observed (open gray circles with error bars) and predicted center-to-limb variation of the equivalent width of the Oi 777.19-nm triplet line as a function of viewing angle ...

Figure 6: (a) The derived Fei (blue circles) and Feii (red circles) abundances (Scott et al., in preparation) as a function of excitation potential of the lower level when using a 3D hydrodynamical so...

Figure 7: Difference between the logarithmic abundances determined from the solar photosphere and the CI carbonaceous chondrites as a function of atomic number. With a few exceptions, the agreement is...

Figure 8: The differences between the helioseismic and predicted sound speeds cs as a function of depth (Serenelli et al., in preparation). The standard solar models shown here only differ in the assu...

Figure 1: Bob and Annie Dicke with their first child, Nancy, in Cambridge, Massachusetts, in 1945. This is about the time Bob was moving from the MIT Radiation Laboratory to the Department of Physics ...

Figure 2: From left to right: Dave Wilkinson, Bob Dicke, Ed Groth, and Jim Peebles in February 1981 on the occasions of a celebration of the Nobel Prize award to Val Fitch and Jim Cronin and the Ph.D....

Figure 3: A photograph I took of Zel'dovich and his wife in Hungary in 1987 on the occasion of IAU Symposium 130. I met Zel'dovich only twice, at this meeting and in 1977 at IAU Symposium 79 in Estoni...

Figure 4: A photograph I took of Donald Shane when he visited Princeton in about 1976. Some of the people who worked on the Lick data reduction are Jim Fry (center left), Ray Soneira (center right), a...

Figure 1: The cosmology school in the new observatory in Tõravere in July 1962. In the center of the second row in a beret is Yakov Zel'dovich. (Photo courtesy of author's archive.)

Figure 2: Discussing galactic models with Sergei Kutuzov (standing) and Grigori Kuzmin (center) in the mid-1960s. (Photo courtesy of author's archive.)

Figure 3: Skiing with Yakov Zel'dovich at the Soviet 6-m telescope, Special Astrophysical Observatory. His wife and Arthur Chernin held my skis and poles. (Photo courtesy of author's archive.)

Figure 4: Jaan Einasto sitting on a mountain ridge near the Soviet 6-m telescope, Special Astrophysical Observatory, in the Caucasus. In the background looms Mount Elbrus, the highest mountain in Euro...

Figure 5: My collaborators (a) Enn Saar and (b) Mihkel Jõeveer in the 1980s. (Photo courtesy of author's archive.)

Figure 6: Distribution of particles in 2D simulations. Figure adapted from Doroshkevich et al. (1976) with permission.

Figure 7: (a) The distribution of Zwicky clusters of the distance class “near” in the Perseus area of the sky in redshift interval 3, 500⩽V0<6, 500 km s−1 and (b)6, 500⩽V0<10, 000 km s−1. Contours of ...

Figure 8: A wedge diagram for the (a) 30°–45° declination zone and (b) 15°–30° declination zone. Filled circles show rich clusters of galaxies, open circles show groups, dots show galaxies, and crosse...

Figure 9: (a) The maximal length LM of connected regions as a function of neighborhood radius R for four catalogs: O, observed; A, adiabatic model; H, hierarchical clustering model; and P, Poisson mod...

Figure 1: (a) Sensitivity to star formation versus redshift for deep survey data at various wavelengths. The key at right indicates the wavelengths and the corresponding flux limits. Most of these lim...

Figure 2: (a) Time dependence of the UV luminosity of an SSP with initial mass 1M⊙, formed with a Salpeter IMF in the range 0.1−100M⊙, measured at three wavelengths, 1,500 Å, 2,300 Å, and 2,800 Å, and...

Figure 3: Age and metallicity dependence of the SFR to UV luminosity ratio (= ) (Equation 10) for a stellar population with a Salpeter IMF in the range 0.1−100M⊙, using the spectral population synthes...

Figure 4: (a) The ratio of SFR/LFUV conversion factors (Equation 10) for Chabrier or Kroupa IMFs to that for a Salpeter IMF (0.1 to 100M⊙), for a constant SFR and for various metallicities computed w...

Figure 5: The SFR to luminosity ratio for dusty galaxies, in solar luminosity units, calibrated with the FSPS models of Conroy et al. (2009), assuming a constant SFR, a Salpeter IMF, and solar metall...

Figure 6: Relative sizes of the regions on the sky observed in several important surveys of the distant Universe. The two Great Observatories Origins Deep Survey (GOODS) fields, the Subaru Deep Field ...

Figure 7: (a) Redshift evolution of the FUV luminosity function at 0<z<4. The colored bands indicate the 68% confidence intervals on the space densities over the observed luminosities (uncorrected for...

Figure 8: (a) SFR densities in the FUV (uncorrected for dust attenuation) and in the FIR. The data points with symbols are given in Table 1. All UV and IR luminosities have been converted to instantan...

Figure 9: The history of cosmic star formation from (a) FUV, (b) IR, and (c) FUV+IR rest-frame measurements. The data points with symbols are given in Table 1. All UV luminosities have been converted ...

Figure 10: The cosmic core-collapse supernova rate (CC SNR). The data points are taken from Li et al. (2011) (cyan triangle), Mattila et al. (2012) (red dot), Botticella et al. (2008) (magenta triangl...

Figure 11: The evolution of the stellar mass density. The data points with symbols are given in Table 2. The solid line shows the global stellar mass density obtained by integrating the best-fit insta...

Figure 12: “Stellar archaeology” with the SDSS. (a) Normalized distribution of stellar mass in the local Universe as a function of age. The red histogram shows estimates from the SDSS (Gallazzi et al....

Figure 13: The mean specific star-formation rate (sSFR≡SFR/M∗) for galaxies with estimated stellar masses in the range 109.4−1010M⊙. The values are from Daddi et al. (2007) (cyan triangle), Noeske et ...

Figure 14: Mean metallicity of the Universe (in solar units): (solid curve) mass of heavy elements ever produced per cosmic baryon from our model SFH, for an assumed IMF-averaged yield of y = 0.02; (t...

Figure 15: Comparison of the best-fit star-formation history (thick solid curve) with the massive black hole accretion history from X-ray [red curve (Shankar et al. 2009); light green shading (Aird et...

Figure 16: (a) Metallicity dependence of the ionizing photon yield, Iion, for a stellar population with a Salpeter IMF (initial mass function) and constant star-formation rate. The points show the val...