adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The L iso − Γ correlation and the E iso/E k − η/Γ correlation for the selected extremely high-efficiency GRBs (ϵ  γ  ≳ 80%). (a) The correlation of L iso and Γ. Obviously, the tight correlation of ﹩{\rm{\Gamma }}\propto {({L}_{\mathrm{iso}})}^{0.29}﹩ (red stars; reduced χ 2 = 0.007) is found, which is consistent with the prediction of the neutrino annihilation from the hyperaccretion disk, ﹩{\rm{\Gamma }}\propto {({L}_{\mathrm{iso}})}^{7/27}={({L}_{\mathrm{iso}})}^{0.26}﹩. Thus, the jet is likely to be thermal-dominated. The dashed cyan line shows the L iso − Γ correlation found in Lü et al. (2012; reduced χ 2 = 0.038, for the large Γ sample of green circles; Xue et al. 2019). (b) The correlation of E iso/E k and η/Γ. A significant linear correlation is found, and it is almost the same when we take E k,52 = 5*L X,45 (reduced χ 2 = 0.138). This is consistent with the E iso/E k = η Mc 2/ΓMc 2 = η/Γ predicted by the photosphere emission model in the unsaturated acceleration regime.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: Evidence from the short GRBs (see Table 8). (a) The different distributions of E p and E iso for the two distinguished samples: ϵ  γ  ≳ 50% (red stars) and ϵ  γ  ≲ 50% (blue stars). (b) The distribution of E ratio and E iso/E k for the ϵ  γ  ≲ 50% sample (reduced χ 2 = 0.140). (c) The E p and E iso distributions of the main pulse for seven other bursts (blue circles and boxes) that have extended emission (see Minaev & Pozanenko 2020) and lack efficiency. Note that the five bursts of the ϵ  γ  ≳ 50% sample (red stars) all have extended emission, including GRB 170817A. (d) A comparison of the ratios of E p and the fluence (or E iso) for the main pulse and the extended emission of a large extended emission sample (reduced χ 2 = 0.196), including the bursts without redshift (blue stars).
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The similar observed efficiency (with E iso/E k from the X-ray afterglow) and theoretically predicted efficiency (from the prompt emission) for the bursts before GRB 110213A (with L X,11h as given in D’Avanzo et al. 2012). (a) The distribution of E ratio and E iso/E k for the ϵ  γ  ≲ 50% sample, which is found to be centered around the equal-value line and have a linear correlation (reduced χ 2 = 0.160). (b), (c) The X-ray afterglow light curves for the bursts (seven bursts) with almost the same E ratio and E iso/E k (see Table 5). We find that all these light curves have a power-law shape with a slope of ∼−1.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The tight correlation of Γ ∝ ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}﹩, predicted by ﹩{\rm{\Gamma }}\propto {E}_{\mathrm{iso}}^{1/8}{E}_{{\rm{p}}}^{1/2}/{\left({T}_{90}\right)}^{1/4}﹩ and ﹩{E}_{{\rm{p}}}\propto {({E}_{\mathrm{iso}})}^{1/4}﹩. (a) The distributions of E p − Γ (red circles; reduced χ 2 = 0.013), E p − η (red triangles; reduced χ 2 = 0.002), and ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}-{\rm{\Gamma }}﹩ (red stars; reduced χ 2 = 0.002) for the selected ϵ  γ  ≳ 50% sample with ﹩{T}_{p}^{}﹩ detections (seven bursts in Figure 2(e); see Table 3). It is obvious that the tight correlations of ﹩{\rm{\Gamma }}={10}^{-0.1}\cdot {E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}﹩ and E p ∝ η (for the five bursts with higher efficiency, thus ﹩\eta \propto {({E}_{\mathrm{iso}})}^{1/4}﹩) are found. (b) The distributions of ﹩({E}_{{\rm{p}}}/{E}_{\mathrm{ratio}})/{\left({T}_{90}\right)}^{1/4}-{\rm{\Gamma }}﹩ (blue circles; reduced χ 2 = 0.031) and ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}-{\rm{\Gamma }}﹩ (cyan triangles) for the selected ϵ  γ  ≲ 50% sample with ﹩{T}_{p}^{}﹩ detection (six bursts in Figure 2(d); see Table 2). The tight correlation of ﹩({E}_{{\rm{p}}}/{E}_{\mathrm{ratio}})/{\left({T}_{90}\right)}^{1/4}\propto {\rm{\Gamma }}﹩ is found, which is in line with the ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}\propto {\rm{\Gamma }}﹩ correlation for the ϵ  γ  ≳ 50% case. (c) The distribution of Γ − ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}﹩ (blue circles; reduced χ 2 = 0.025) for the large sample with Γ (47 bursts; see Table 6) in Ghirlanda et al. (2018). For the ϵ  γ  ≳ 50% case, the ﹩{E}_{{\rm{p}}}^{}﹩ is rederived from the ﹩\mathrm{log}﹩ (E p) ﹩=\,2.54+0.25\mathrm{log}﹩ (E iso) correlation (using E iso), and for the ϵ  γ  ≲ 50% case, the ﹩{E}_{{\rm{p}}}^{}﹩ is rederived from E p/E ratio. Obviously, we find that the distribution of Γ and ﹩{E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}﹩ is centered around ﹩{\rm{\Gamma }}={10}^{-0.1}\cdot {E}_{{\rm{p}}}^{}/{\left({T}_{90}\right)}^{1/4}﹩ and has a linear correlation.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The L iso − Γ and E iso − L X,45 distributions for the ϵ  γ  = 50% sample (see Table 7). (a) The distribution of L iso and Γ for the complete sample (62 bursts) with the detection of T  p . We select the sample (nine bursts, marked by the red pluses) with the maximum Γ (for fixed L iso) to check whether their efficiency is 50%, as predicted by the photosphere emission model. (b) The distribution of E iso and L X,45 for the selected sample with the maximum Γ (four bursts with L X,45 detection, marked by the red stars). It is found that all these bursts have almost the same efficiency (with E iso ∝ L X ∝ E k, reduced χ 2 = 0.008 ). Thus, we think that the efficiency ϵ  γ  for these bursts is likely to be 50% (E iso,52 = E k,52 ≃ 3.7 ∗ L X,45).
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The distribution of E iso/E k for our whole sample (117 bursts, after GRB 110213A; see Tables 1–3). The mean value is around ∼10−0.2–10−0.3, thus indicating the average efficiency of ϵ  γ  ∼33%–40%. The distribution also seems to consist of three Gaussian distributions (smaller χ 2 for E iso/E k ≳ 10−1.0).
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The optical afterglow light curves for six extremely high-efficiency GRBs (ϵ  γ  ≳ 80%) whose early peaks can be detected. All these light curves show significant reverse shock signals. (a) Three GRBs that are also considered to have reverse shock signals (with detections of both the rapid rise f ≳ ﹩{t}_{}^{3}﹩ and the fall f ∼ ﹩{t}_{}^{-2}﹩) in other works (Gao et al. 2015; Yi et al. 2020). (b) Three GRBs with detections of only the rapid rise f ≳ ﹩{t}_{}^{3}﹩ or the rapid fall f ∼﹩{t}_{}^{-2}﹩.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The E p evolutions of the time-resolved spectra for five extremely high-efficiency GRBs (ϵ  γ ≳ 80%) detected by Fermi/GBM. The E p evolutions almost follow the evolution of the flux F, consistent with the E p ∝ F 1/4 predicted by the photosphere (thermal) emission in the unsaturated acceleration regime.
Paper: Evidence of Photosphere Emission Origin for Gamma-Ray Burst Prompt Emission
Authors: Yan-Zhi Meng
Figure caption: The X-ray afterglow light curves for the selected extremely high-efficiency GRBs (excluding GRB 990705 and GRB 000210). All these light curves appear as simple power-law shapes, without any plateaus, steep decays, or significant flares (with weak flares in the early times).
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Footprint of the HST observations, superimposed on the Spitzer/IRAC 3.6 μm data of four Frontier Fields clusters (Lotz et al. 2017). The ALCS band 6 ALMA coverage is shown as the shaded orange areas. The images shown cover both the cluster and the parallels of the HFF.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The arrangement of all available HST filters within ALCS clusters. These filters include (top to bottom): seven broad bands from WFC3/UVIS (e.g., f275wu), eight bands from ACS/WFC, five broad bands from WFC3/NIR, and two bands from Spitzer/IRAC.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband magnitude measured in our catalog and Shipley et al. (2018), for the cluster (top) and parallel (bottom) parts of the A370 field. We only compare the objects in the central part of the field. For clarity, the colors of shaded regions correspond to HST/ACS (purple), HST/WFC3 (blue), and Spitzer/IRAC (maroon). The difference in magnitude ΔMag is shown by scattered circles, which are colored based on the density of sources around them. The overlaid solid lines correspond to the binned median, which are selected to contain the same amount of objects in each bin. The shaded envelope captures the 68% of points per magnitude bin. The vertical dashed lines correspond to the 1σ depth limit for each band. The median ΔMag for galaxies brighter than the depth limit is shown on each panel.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Results from the modeling procedure on the relatively crowded A370 cluster field. The cutouts are 30″ across, and were selected to show a wide variety of sources on the same image, i.e., the ones modeled purely with GOLFIR, and the galaxy model refined by using GALFIT. Top: The HST RGB image created from the combination of F814W, F125W, and F160W filters, the HST detection image and segmentation map. Middle: The original IRAC 3.6 μm science image, the GOLFIR model, and residual images. Bottom: Same as above, but now the model was additionally refined with GALFIT. The color scale has been adjusted to show the 3σ range for each image. Most notably, the final residual mosaic can also be used to extract additional IRAC photometry for sources without an HST counterpart. The images are oriented with north up and east to the left.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Image stamps displaying natural and tapered ALMA maps, alongside a cutout from HST/ACS, HST/WFC3, and IRAC for three sources in the SMACS0723 and A2744 fields. On top of each image we overlay 1, 2, and 3σ contours. Green and purple shapes at the bottom of ALMA cutouts represent the size of the beam. Each panel is 10″ across. The remainder of the stamps for each source will be presented in an upcoming work (S. Fujimoto et al. 2022, in preparation) and are also available in the same repository as our catalogs.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Classification of galaxies for all ALCS fields by using the NUV − r and r − J rest-frame colors. The NUV − r − J galaxy selection prescription from Ilbert et al. (2013) is shown as a solid red line. The fraction of quiescent galaxies (QGs) is displayed within each plot. Here we have limited our selection to only include galaxies with nusefilt ≥ 5 and a S/N > 5 in the HST f160w filter.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Red-sequence diagnostic for galaxies within the Hubble Frontier Fields. Left: A histogram of all objects in the catalog in the 0 < z < 1 range (red) and an isolated sample of galaxies which we consider to belong to the cluster (gray), ∣z − z clu∣ < 0.1, and F606W < 25 AB mag. The vertical red line represents the redshift of the cluster. Right: color–magnitude diagnostics of the red sequence with the F435W and F606W filters.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The log-scaled distribution of best-fit photometric redshifts (left) and computed magnification factors (right) for the full catalog. The median and the 68% confidence interval for each parameter are shown on each plot.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Comparison between photometric redshifts derived by EAZY and the spectroscopic redshift from the literature. We have carried out the comparison in all fields where a match was found; in total, these include all five Frontier Fields, 10 CLASH fields, and nine RELICS field. Black and red circles denote galaxies below and above the catastrophic limit of 0.15, respectively.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband color computed in our catalog and Shipley et al. (2018), for the cluster (top) and parallel (bottom) parts of the A370 field. The colors and symbols are the same as those in Figure 10.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: A density plot of EAZY-derived demagnified stellar mass as a function of redshift. ALMA-detected galaxies are shown as blue diamonds. A bright, multiply lensed z = 6.07 source from Fujimoto et al. (2021) is shown as a purple star.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: (Left) Sky distributions of 23 Fornax cluster galaxies with CO detections. The spatial size of CO data (moment 0) is enlarged by a factor of 30. The linear scaling is adopted for plotting the moment 0 map of the CO-detected galaxies except for NGC 1365, for which the logarithmic scaling is adopted. Background is the X-ray image obtained by combining the Suzaku and XMM-Newton data for the Fornax cluster (Murakami et al. 2011). (Right) Stellar mass vs. SFR relation of our sample galaxies. Moment 1 maps of the CO-detected galaxies are shown. The white solid line and shaded region indicate the star-forming main sequence of Speagle et al. (2014) and its standard deviation, respectively.
Paper: CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
Authors: Kana Morokuma-Matsui, Kenji Bekki, Jing Wang, Paolo Serra, Yusei Koyama, Tomoki Morokuma, Fumi Egusa, Bi-Qing For, Kouichiro Nakanishi, Bärbel S. Koribalski, Takashi Okamoto, Tadayuki Kodama, Bumhyun Lee, Filippo M. Maccagni, Rie E. Miura, Daniel Espada, Tsutomu T. Takeuchi, Dong Yang, Minju M. Lee, Masaki Ueda, Kyoko Matsushita
Figure caption: (Left) Sky distributions of Fornax cluster galaxies. Our entire ACA sample and those with H I mass measurements (including upper limits) are indicated with blue open squares or orange X marks, respectively. Those with M star > 109 M ⊙ are indicated with blue filled squares. The gray open circles indicate the FCC galaxies (Ferguson 1989a). The purple contours indicate the X-ray distribution obtained with the Suzaku and XMM-Newton data (Murakami et al. 2011). Our ACA sample is distributed over the region where the FCC galaxies are distributed. (Right) Stellar mass vs. SFR relation of our sample galaxies. The gray solid line and gray shaded region indicate the main sequence of star-forming galaxies defined in Speagle et al. (2014) and its standard deviation, respectively.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: Top: The area-normalized number counts in the F814W and F160W filters for the central part of the A370 cluster and parallel fields. We show the number counts for our catalog as black squares, while the Shipley et al. (2018) work is overplotted in blue circles. Bottom: The area-normalized number counts in the F814W and F160W filters for the central part of the MACSJ0416 cluster and parallel fields. We show the number counts for our catalog as black squares, while the ASTRODEEP data are overplotted in blue circles.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband magnitude computed in our catalog compared to CLASH photometric catalog of Molino et al. (2017). The colors and symbols are the same as those in Figure 10.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband color computed in our catalog compared to CLASH photometric catalog of Molino et al. (2017). The colors and symbols are the same as those in Figure 10.
Paper: ALMA Lensing Cluster Survey: Hubble Space Telescope and Spitzer Photometry of 33 Lensed Fields Built with CHArGE
Authors: V. Kokorev, G. Brammer, S. Fujimoto, K. Kohno, G. E. Magdis, F. Valentino, S. Toft, P. Oesch, I. Davidzon, F. E. Bauer, D. Coe, E. Egami, M. Oguri, M. Ouchi, M. Postman, J. Richard, J.-B. Jolly, K. K. Knudsen, F. Sun, J. R. Weaver, Y. Ao, A. J. Baker, L. Bradley, K. I. Caputi, M. Dessauges-Zavadsky, D. Espada, B. Hatsukade, A. M. Koekemoer, A. M. Muñoz Arancibia, K. Shimasaku, H. Umehata, T. Wang, W.-H. Wang
Figure caption: The difference between broadband magnitude measured in our catalog and the ASTRODEEP data, for the cluster (top) and parallel (bottom) parts of the MACSJ0416 field. Symbols and colors are the same as those in Figure 10.