adsabs/AstroCLIMB huggingface dataset:
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent image of an equatorial thin disk in the Kerr BH spacetime with a = 0.995 (﹩[{a}_{({\ell },\gamma ,\epsilon )}^{-},1]﹩), with r inner = 1.2219134 and ﹩{r}_{\mathrm{outer}}={r}_{\epsilon }^{+}=2﹩ where ℓ = ℓ − = 2.1004. It refers to the analysis of Figure C15. Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent image of an equatorial thin disk in the Kerr BH spacetime with a = 0.999. See Figure C17. Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩. Where r inner = 1.0934, with r outer = 2.0081, and ℓ = 2.04484 (disk model (a)).
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent (redshift) image of an equatorial thin disk in the Kerr BH spacetime with a = 0.9. See Figure C13. There is (r inner = 2, r outer = 3.76166, r center = 2.77723, ℓ = 2.51602). Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH with spin a = 0.81 (class (3)(ii) for ﹩a\in [{a}_{\gamma }^{\epsilon },{a}_{(b,\epsilon )}^{-}[﹩—see Table 2) of Section 4.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH with spin a = 0.9 (class (4) for ﹩a\in [{a}_{({\ell },\gamma ,b)}^{\mp },{a}_{({\ell },\gamma ,\gamma )}^{\mp }[﹩—see Table 2) of Section 4.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH with spin a = 0.995 (class (5)(iv) for ﹩[{a}_{({\ell },\gamma ,\epsilon )}^{-},1]﹩—see Table 2) of Section 4.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH with spin a = 0.999 (class (5)(iv) for ﹩a\in [{a}_{({\ell },\gamma ,\epsilon )}^{\mp },1[﹩ ; see Table 2). Disk model (c) in the left panel has (r inner = 1.07, r outer = 6.81754, ℓ = 2.05818).
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH with spin a = 0.999 (class (5)(iv)). Disk model (b) in left panel has (r inner = 1.075066, r outer = 4.00089, ℓ = 2.05445). Angle views σ = 0.99 (pink line central panel) and σ = 0.95 (cyan line and right panel) are shown.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent image of an equatorial thin disk in the Kerr BH spacetime with a = 0.999. It refers to the analysis of Figure C21, for disk model (c), having (r inner = 1.07, r outer = 6.81754, ℓ = 2.05818). Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent image of an equatorial thin disk in the Kerr BH spacetime with a = 0.999. It refers to the analysis of Figure C19, for disk model (b), having (r inner = 1.075066, r outer = 4.00089), and ℓ = 2.05445. Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Apparent image of an equatorial thin disk in the Kerr BH spacetime with a = 0.999. It refers to the analysis of Figure C23, for disk model (d), having (r inner = 1.16, r outer = 1.23673, ℓ = 2.03292). Each panel is for a different view angle ﹩\sigma \equiv {\sin }^{2}\theta ﹩.
Paper: Photon Shells, Black Hole Shadows, and Accretion Toroids
Authors: D. Pugliese, Z. Stuchlík
Figure caption: Analysis of Figure C8 for a BH spin a = 0.999 and class (5) of Section 4. Disk model (d) in the left panel has (r inner = 1.16, r outer = 1.23673, ℓ = 2.03292).
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: False color image of AUDFs. Red refers to the HST/ACS/F606W image, green is the N242W filter, and blue is the F154W filter of UVIT on board AstroSat. HST and N242W images are convolved with F154W PSF and have the same pixel scale as in the F154W band. The zoom-in portion (A, B, and C) of the image is shown to highlight the imaging quality and astrometric accuracy of the two UVIT filters. Region B refers to one of the blue squares from HUDF.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: UVIT/AstroSat observational layout under the GT05-240 proposal. CDFS-I (53.03394, −27.91539) and CDFS-II (53.25806, −27.68067) are the two pointing planned for 50 ks on-source observation each in the F154W and N242W filters. The blue tiles represent the HUDF (S. V. W. Beckwith et al. 2006); each small box has a size of ﹩1{\rm{^{\prime} }}\times 1{\rm{^{\prime} }}﹩. The green region inside HUDF is known as the Hubble XDF (G. D. Illingworth et al. 2013). The background image is from the GALEX NUV deep field (D. C. Martin et al. 2005).
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Difference between the coordinate of a star in the Gaia EDR3 catalog and its location on the N242W image. The orange solid histograms represent the difference in R.A. and decl. for the stars that belong to the GOODS South region only, while black histograms are for the entire field (CDFS-I and CDFS-II). The blue dots represent the same but for randomly selected bright (N242Wmag2 <26.5) objects with their unique counterparts marked as HLFflag = 1 in the AUDFs-N242W-Cat1-v1 catalog. The rms difference for the GOODS South region is 0.″13 and 0.″18 along R.A. and decl., respectively. While for the entire region, they are 0.″38 and 0.″34, respectively. The green square represents one UVIT pixel.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Upper panel: CDFS-II field final image in the F154W, N242W filters (see Figure 1 for reference). In the bottom panels are shown the VIS3 (V461W) channel image in a single frame and the effective area curves as a function of wavelength for the three filters used for observations. The filter's effective area is derived by multiplying the filter transmission curve with the quantum efficiency of the detector.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Brief outline of the U2LP pipeline and key processes involved in creating the orbitwise images in F154W and N242W filters. Inset figure shows the Relative Aspect Series (satellite drift correction) derived from the V461W (VIS3) channel for a single orbit.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Left: Cosmic IR SFRD measurements from ALCS IR LFs at z = 0.6–7.5. The red circles are our measurements with a conversion of SFR [M ⊙ yr−1] = 4.5 × 10−44 L IR [erg s−1], which is the same calibration as those from Madau & Dickinson (2014), but we multiply a factor of 0.63 to apply the correction from the Salpeter IMF to the Chabrier IMF. In both panels, the filled and open red circles indicate the integration range of IR LFs down to our detection limit of L IR = 1010 L ⊙ and the potential turnover or flattening IR luminosity of L IR = 108 L ⊙ (see Section 6.3). The black solid and dashed lines are two empirical models of “Dust Rich” and “Dust Poor” scenarios presented in Casey et al. (2018a), respectively. The gray shaded region denotes previous measurements of Zavala et al. (2021) that perform a backward evolution model to constrain the evolution of the IR LFs to reproduce the observed number counts at 1.2 and 3 mm. The gray line is the prediction from the SHARK simulation (Lagos et al. 2018, 2020), where the integrated L IR range is matched with our measurements. Right: Cosmic total (= IR + UV) SFRD measurements. The black line shows the previous best estimate of the empirical model (Equation (9)) fitting to the SFRDtotal and SFRDcorr measurements presented in Madau & Dickinson (2014). The blue and brown shaded regions present the 1σ range of the previous SFRDUV estimates without and with the dust correction, respectively, drawn by fitting the empirical model (Equation (9)) to the measurements presented in Bouwens et al. (2020). The red filled circles represent our SFRDtotal measurements estimated from our SFRDIR and the previous SFRDUV estimate without the dust correction (Bouwens et al. 2020). The red line and shaded region are the best-fit empirical model (Equation (9)) for our SFRDtotal measurements and its 1σ range. For presentation purposes, we slightly shift the open red circles along the abscissa.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: ALCS IR LF measurements at z = 0.6–7.5. The red-filled circles represent our ALCS sources corrected from the MC simulations that implement all relevant uncertainties, such as redshift, magnification, and flux density measurements, where the error bars indicate the 16–84th percentile in the 1000 MC realizations (see Section 5.1). Previous IR LF measurements with Herschel (Gruppioni et al. 2013; Magnelli et al. 2013; Wang et al. 2019a) and ALMA(+SCUBA2) are presented in gray and colored symbols, respectively. The red line presents the best-fit DPL functions, where we include our measurements and other ALMA blind survey results (Koprowski et al. 2017; Hatsukade et al. 2018) in the fitting. The other color lines show the predictions from simulations (Lagos et al. 2020; Trayford et al. 2020; Bethermin et al. 2022; Vijayan et al. 2022) and an empirically calibrated model (Zavala et al. 2021).
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Comparison of differential number counts at 1.2 mm among different subsamples of ALCS clusters. The red circles and line are the same assignments with Figure 9. The open blue, orange, and green circles and lines indicate the number counts and their best-fit Schechter functions derived only with the HFF, CLASH, and RELICS clusters, respectively. The red and gray shaded regions represent the 1σ areas evaluated with the Bootstrap tests by sampling 33 clusters from all ALCS clusters (including the duplication) and only five clusters from the CLASH and RELICS clusters, respectively. The blue circles and upper limits denote the previous ALMA Band 6 survey results in HFF (Muñoz Arancibia et al. 2023), where the data are shallower than ALCS.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Impact of the completeness correction from different intrinsic size distributions. Left: Faint end of the number counts. The red open circles and solid line are the same assignments as Figure 9 based on the constant size assumption for the dust continuum emission. The blue and green circles and solid lines show the number counts and the best-fit Schechter functions obtained by rerunning the same MC simulations for the corrections of the completeness and flux measurements with the assumptions of the negative (e.g., González-López et al. 2017a; Smail et al. 2021) and positive (Fujimoto et al. 2017, 2018) correlations between L IR and the dust continuum size, respectively. Right: integration of the 1.2 mm number counts down to our detection limit according to the best-fit Schechter functions with the different size assumptions for the dust continuum emission, suggesting that the resolved fraction of the CIB at 1.2 mm could change by factors of ∼0.6–1.1 due to the different size assumptions.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Zoom-in spectra of the 27 GHz wide (∼85–112 GHz) follow-up ALMA Band 3 line cube (left) and the ALCS 15 GHz wide Band 6 line cube (right) for a NIR-dark lensed galaxy of M0553-C67. The Band 3 follow-up line-scan observations yield a robust single line detection (S/N = 12.1) at ∼97.1 GHz. Based on the photometric redshift of z phot ≳ 4 and the nondetection of neighboring lines, we regard the line as CO(5–4) at z = 4.93 in this paper (see Appendix A). The blue and green dashed vertical lines indicate the line frequency of [C I](1-0) at z = 3.74 and [C II]158μm at z = 6.12 in case the 97.1 GHz line corresponds to CO(4–3) and CO(6–5), respectively.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Evolution of Φ⋆ (left) and L ⋆ (right). The red circles are our IR LF measurements with the best-fit DPL functions (Table 8). We note in our measurements that all parameters in the DPL function are free in the fitting for the z = 1.0–2.0 bin, while the bright-end (and faint-end) slope is fixed for the other bins. For comparison, we also show the previous measurements with Herschel (Gruppioni et al. 2013; Magnelli et al. 2013; Wang et al. 2019a), SCUBA2 (Lim et al. 2020), and SCUAB2+ALMA (Koprowski et al. 2017). The magenta solid and dashed lines are the best-fit measurements presented in Koprowski et al. (2017) and their extrapolations, respectively.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Example of our template fitting for the ALCS sources with no HST counterparts. Left: the best-fit SEDs for M0417-C121 based on the templates of Arp220 (black line) and the composite of 707 dusty galaxies in AS2UDS (Dudzevičiūtė et al. 2020). Right: P(z) from the χ 2 minimization. The red dashed line indicates z spec = 3.652 of M0417-C121 determined from follow-up ALMA Band 3 and 4 line-scan observations with multiple line detection (Tsujita et al. 2024).
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Evolution of IR LFs based on our best-fit DPL functions presented in Figure 15. We find the overall trends characterized by the positive luminosity evolution coupled with the negative density evolution.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: ALCS Band 6 continuum-subtracted spectra for the 10 serendipitous line detection in the ALCS continuum sources. The S/N, central frequency, and line width are summarized in Table 9.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption:                         Same as Figure 26, but for 39 ALCS sources in the prior catalog.