adsabs/AstroCLIMB huggingface dataset:
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at z ∼ 5.5
Authors: Yunjing Wu, Feige Wang, Zheng Cai, Xiaohui Fan, Kristian Finlator, Jinyi Yang, Joseph F. Hennawi, Fengwu Sun, Jaclyn B. Champagne, Xiaojing Lin, Zihao Li, Zuyi Chen, Eduardo Bañados, George D. Becker, Sarah E. I. Bosman, Gustavo Bruzual, Stephane Charlot, Hsiao-Wen Chen, Jacopo Chevallard, Anna-Christina Eilers, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Mingyu Li, Weizhe Liu, Maria A. Pudoka, Wei Leong Tee, Zhang-Liang Xie, Siwei Zou
Figure caption: Best SED solution based on BEAGLE. The photometric data points from HST+ JWST are represented by blue triangles, while the corresponding model photometries are shown in red. The median value of the posterior distribution of SEDs is shown with the black line. The gray region represents the 16th and 84th confidence intervals.
Paper: The Gas Accretion Rate of Star-forming Galaxies over the Last 4 Gyr
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: The time-averaged SFR (dashed red curve), the average net molecular gas formation rate (dashed blue curve), and the average net gas accretion rate of the disks of present-day main-sequence galaxies (dashed black curve) over the past 4 Gyr are shown as functions of their present-day stellar mass (M *,0, bottom axis) and their initial stellar mass (M *,0.35, top axis). The dotted curves show the results for the average rates on extrapolating the H I scaling relation of Bera et al. (2023) to a stellar mass of M * = 1010.7 M ⊙ at z ≈ 0.35. The star indicates the average met gas accretion rate for galaxies with stellar masses equal to that of the Milky Way. The shaded regions show the 68% confidence intervals for the average net gas accretion rate and the average net molecular gas formation rate.
Paper: The Gas Accretion Rate of Star-forming Galaxies over the Last 4 Gyr
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: Fractional changes, with respect to their respective present-day values, in the average (a) stellar mass (ΔM */M *,0), (b) molecular gas mass (ΔM mol/M mol,0), and (c) atomic gas mass (ΔM atom/M atom,0) in the disks of main-sequence galaxies from z ∼ 0.35 to z ∼ 0 are shown as functions of their present-day stellar mass (M *,0, bottom axis) and their initial stellar mass (M *,0.35, top axis). The shaded regions show the 68% confidence intervals.
Paper: The Gas Accretion Rate of Star-forming Galaxies over the Last 4 Gyr
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: Net changes in the average (a) stellar mass (M *), (b) molecular gas mass (M mol), and (c) atomic gas mass (M atom) in the disks of main-sequence galaxies from z ∼ 0.35 to z ∼ 0 are shown as functions of their present-day stellar mass (M *,0, bottom axis) and their initial stellar mass (M *,0.35, top axis). The shaded regions show the 68% confidence intervals.
Paper: The Gas Accretion Rate of Star-forming Galaxies over the Last 4 Gyr
Authors: Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla
Figure caption: (a) Net change in the average baryonic mass (ΔM baryon ≡ M acc) in the disks of main-sequence galaxies from z ∼ 0.35 to z ∼ 0 as a function of their present-day stellar mass (M *,0, bottom axis) and their initial stellar mass (M *,0.35, top axis). (b) The fractional change in the average baryonic mass, with respect to the present-day baryonic mass, as a function of the present-day stellar mass (bottom axis) and the initial stellar mass (top axis). The shaded regions in the figures show the 68% confidence intervals for the corresponding curves.
Paper: Fast Radio Bursts: Electromagnetic Counterparts to Extreme Mass-ratio Inspirals
Authors: Rui-Nan Li, Zhen-Yin Zhao, Zhifu Gao, Fa-Yin Wang
Figure caption: The effective GW strain of EMRI events (dots) and the sensitivity curves ﹩\sqrt{{{fS}}_{n}(f)}﹩ of LISA and Tianqin (solid lines). Two mission times for LISA are considered (Wagg et al. 2022a, 2022b). Panels (a) and (b) correspond to cases 1 and 2 in Table 2, respectively.
Paper: Fast Radio Bursts: Electromagnetic Counterparts to Extreme Mass-ratio Inspirals
Authors: Rui-Nan Li, Zhen-Yin Zhao, Zhifu Gao, Fa-Yin Wang
Figure caption: The effective GW strain of EMRI events (dots) and the sensitivity curves ﹩\sqrt{{{fS}}_{n}(f)}﹩ of LISA and Tianqin (solid lines). Two mission times for LISA are considered (Wagg et al. 2022a, 2022b). The numbers and colors denote different cases listed in Table 1.
Paper: Fast Radio Bursts: Electromagnetic Counterparts to Extreme Mass-ratio Inspirals
Authors: Rui-Nan Li, Zhen-Yin Zhao, Zhifu Gao, Fa-Yin Wang
Figure caption: The effective GW strain of EMRI events (dots) and the sensitivity curves ﹩\sqrt{{{fS}}_{n}(f)}﹩ of LISA and Tianqin (solid lines). Two mission times for LISA are considered (Wagg et al. 2022a, 2022b). Panels (a) and (b) correspond to cases 1 and 2 in Table 1 when the orbital evolution is considered. The redshift of panel (a) is set to 0.08, and the redshift of panel (b) is set to 0.2.
Paper: An ALMA-resolved View of 7000 au Protostellar Gas Ring around the Class I Source CrA-IRS 2 as a Possible Sign of Magnetic Flux Advection
Authors: Kazuki Tokuda, Naofumi Fukaya, Kengo Tachihara, Mitsuki Omura, Naoto Harada, Shingo Nozaki, Ayumu Shoshi, Masahiro N. Machida
Figure caption: (a) An average C18O spectrum toward IRS 2 over the region where the 1.3 mm continuum mission is larger than 0.05 Jy beam−1. The red dashed line represents the systemic velocity, 6.4 km s−1, of the protostar judging from the dip velocity. (b) A C18O position–velocity (PV) diagram toward over the ring structure. We extracted the spectral cube along the rectangle with a length of 70″ and a width of 55″ at the same central coordinate of the ring center as shown in Figure 1. The y-axis shows the decl. offset from the center. The cyan dotted lines along the horizontal axis denote the ring radius as shown in Figure 1. The white dotted line represents the systemic velocity defined in panel (a).
Paper: An ALMA-resolved View of 7000 au Protostellar Gas Ring around the Class I Source CrA-IRS 2 as a Possible Sign of Magnetic Flux Advection
Authors: Kazuki Tokuda, Naofumi Fukaya, Kengo Tachihara, Mitsuki Omura, Naoto Harada, Shingo Nozaki, Ayumu Shoshi, Masahiro N. Machida
Figure caption: (Left panel) The color-scale image shows the velocity-integrated intensity (moment 0) map of C18O (2–1) with a velocity range of 5–7 km s−1. The white contours show the 1.3 mm continuum image with contour levels of 0.05, 0.15, and 0.25 Jy beam−1. The synthesized beam size, 2.″1 × 1.″3 is given by the white ellipse at the lower left corner. The white dashed circle highlights the ring structure with a radius of 25″ (∼3700 au) at a central coordinate of (α J2000.0, δ J2000.0) = (19h01m39.ˢ13, −36°58′47.″3). (Right panel) The color-scale image shows the velocity-field (moment 1) map toward IRS 2. The contours and circle are the same as in the right panel.
Paper: An ALMA-resolved View of 7000 au Protostellar Gas Ring around the Class I Source CrA-IRS 2 as a Possible Sign of Magnetic Flux Advection
Authors: Kazuki Tokuda, Naofumi Fukaya, Kengo Tachihara, Mitsuki Omura, Naoto Harada, Shingo Nozaki, Ayumu Shoshi, Masahiro N. Machida
Figure caption: C18O (2–1) velocity-channel maps toward the ring structure around IRS 2 are shown in color-scale images. The white lines are the same as those in Figure 1. White contours show the SO (NJ  = 56–45) emission with contour levels of 0.9, 1.8, 2.7, and 3.6 K. The yellow crosses demote the peak position of the 1.3 mm continuum image, (α J2000.0, δ J2000.0) = (19h01m41.ˢ58, −36°58′31.″9).
Paper: GRB 221009A: Revealing a Hidden Afterglow during the Prompt Emission Phase with Fermi-GBM Observations
Authors: Hai-Ming Zhang, Yi-Yun Huang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Light-curve data and modeling of GRB 221009A in 50–100 keV and 200–400 keV. Left panel: the three shaded regions represent the time intervals (I, II, and III) that are selected for spectral analysis, as shown in Figures 1, 2, and 3. The blue data points show the flux after fitting the spectra with the best model (Band, PL, or Band+PL model), while the black data points show the flux of the PL component extracted from the spectral analysis. The red lines show the fitting of the black data points with a single PL function, resulting in slopes of −0.94 ± 0.02 and −0.95 ± 0.05 for 50–100 keV and 200–400 keV, respectively. Right panel: the afterglow component of GRB 221009A and modeling with the jet break models. The black lines show the fitting with a BPL function with free α 1 and α 2, the magenta lines show the fitting with a BPL with free α 1 and α 2 = α 1–3/4, and the red lines show the fitting with a BPL with free α 1 and α 2 = −2.0, respectively. The bottom panels show the evolution of the PL photon index in 40–8000 keV.
Paper: GRB 221009A: Revealing a Hidden Afterglow during the Prompt Emission Phase with Fermi-GBM Observations
Authors: Hai-Ming Zhang, Yi-Yun Huang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: (a) The light curve of GRB 221009A in 40–8000 keV as seen by the NaI 4, NaI 8, and BGO 1 of Fermi-GBM during the interval T 0 + [288–328] s. The light blue vertical shaded region shows the BTI (T 0 + [219–277] s) of Fermi-GBM. The light curve is divided into five time slices (A–E, differentiated by the vertical dashed lines) for the spectral analysis. (b–d) The model spectra in ν F  ν  units for all five time slices. The best-fit model for the spectra in slices A and B is the Band function. The best-fit model for the spectrum in slice c is Band+PL function. The best-fit model for the spectra in slices D and E is the PL function.
Paper: GRB 221009A: Revealing a Hidden Afterglow during the Prompt Emission Phase with Fermi-GBM Observations
Authors: Hai-Ming Zhang, Yi-Yun Huang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Same as Figure 1 but for the time interval T 0 + [328–378] s.
Paper: GRB 221009A: Revealing a Hidden Afterglow during the Prompt Emission Phase with Fermi-GBM Observations
Authors: Hai-Ming Zhang, Yi-Yun Huang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Same as Figure 1 but for the time interval T 0 + [514–1467] s.
Paper: GRB 221009A: Revealing a Hidden Afterglow during the Prompt Emission Phase with Fermi-GBM Observations
Authors: Hai-Ming Zhang, Yi-Yun Huang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: An example of the count-rate spectrum (during the interval T 0 + 308–T 0 + 318 s) in comparison with the PL (left panel), Band (middle panel), and Band+PL (right panel) models, respectively. The corresponding statistics for the fits are shown in Table 3 in Appendix.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at z ∼ 5.5
Authors: Yunjing Wu, Feige Wang, Zheng Cai, Xiaohui Fan, Kristian Finlator, Jinyi Yang, Joseph F. Hennawi, Fengwu Sun, Jaclyn B. Champagne, Xiaojing Lin, Zihao Li, Zuyi Chen, Eduardo Bañados, George D. Becker, Sarah E. I. Bosman, Gustavo Bruzual, Stephane Charlot, Hsiao-Wen Chen, Jacopo Chevallard, Anna-Christina Eilers, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Mingyu Li, Weizhe Liu, Maria A. Pudoka, Wei Leong Tee, Zhang-Liang Xie, Siwei Zou
Figure caption: Top left: the JWST/NIRCam WFSS spectrum of ASPIRE-J0305M31-O3-038. The error spectrum is shown in pink lines. Bottom left: normalized X-SHOOTER spectrum of the quasar J0305 with Mg II λ λ2796, 2803 and Fe II λ 2382, 2600 absorptions at z = 5.4284. Red shaded regions denote the best-fit Voigt profile. Dashed blue lines indicate the redshift. Right: JWST/NIRCam composite the red, green, and blue map of the quasar field with the pixel scale of 0.″03 (blue: F115W, green: F200W, red: F356W). White circles denote the location of ASPIRE-J0305M31-O3-038 and the quasar J0305. We note that the Mg II absorber is in front of the quasar with the redshift of z = 5.428. The impact parameter between the Mg II absorber and ASPIRE-J0305M31-O3-038 is 4.″1, corresponding to 24.9 pkpc at z = 5.428.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at z ∼ 5.5
Authors: Yunjing Wu, Feige Wang, Zheng Cai, Xiaohui Fan, Kristian Finlator, Jinyi Yang, Joseph F. Hennawi, Fengwu Sun, Jaclyn B. Champagne, Xiaojing Lin, Zihao Li, Zuyi Chen, Eduardo Bañados, George D. Becker, Sarah E. I. Bosman, Gustavo Bruzual, Stephane Charlot, Hsiao-Wen Chen, Jacopo Chevallard, Anna-Christina Eilers, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Mingyu Li, Weizhe Liu, Maria A. Pudoka, Wei Leong Tee, Zhang-Liang Xie, Siwei Zou
Figure caption: Left: [O III] EWs and derived stellar masses at z ∼ 6, compared to those of local galaxies (shaded region; MPA-JHU catalog (Kauffmann et al. 2003; Brinchmann et al. 2004)). The measurement of the absorber-associated [O III] emitter is shown as the red star. Gray dots indicate results obtained from the EIGER sample (Matthee et al. 2023). Right: SFR distribution of metal-absorber-selected galaxies. Galaxies at z > 5 are marked as hatched bars. At z < 5, the C IV-associated LAEs selected from the MAGG survey (Galbiati et al. 2023) are shown in gray. The blue bars show the C IV-associated LAEs at z > 5 (Cai et al. 2017; Díaz et al. 2021). At z ≈ 6, one ALMA-detected O I-associated emitter is shown in pink (Wu et al. 2021). The [O III] emitter detected with JWST is shown in red.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at z ∼ 5.5
Authors: Yunjing Wu, Feige Wang, Zheng Cai, Xiaohui Fan, Kristian Finlator, Jinyi Yang, Joseph F. Hennawi, Fengwu Sun, Jaclyn B. Champagne, Xiaojing Lin, Zihao Li, Zuyi Chen, Eduardo Bañados, George D. Becker, Sarah E. I. Bosman, Gustavo Bruzual, Stephane Charlot, Hsiao-Wen Chen, Jacopo Chevallard, Anna-Christina Eilers, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Mingyu Li, Weizhe Liu, Maria A. Pudoka, Wei Leong Tee, Zhang-Liang Xie, Siwei Zou
Figure caption: Left: spatial distribution of [O III] emitters relative to the quasar. The location of the quasar is shown with a blue star. Dots represent the locations of [O III] emitters, while the shaded circles correspond to the virial radii of galaxies estimated from their best SED-derived stellar masses. Right: the redshift distribution of [O III] emitters at z < 6 in this quasar field (J0305). The hatched bar indicates [O III] emitters clustering at z ≃ 5.4. Targets at other redshifts (∣dv∣ > 1000 km s−1) are shown in blank bars, ﹩{\rm{\Delta }}v([{{\rm{O}}}_{\mathrm{III}}]-{\mathrm{Mg}}_{\mathrm{II}})=({z}_{[{{\rm{O}}}_{\mathrm{III}}]}-{z}_{{\mathrm{Mg}}_{\mathrm{II}}})/(1+{z}_{{\mathrm{Mg}}_{\mathrm{II}}})\times c﹩. The velocity offsets and impact parameters are shown in the top right panel. The Mg II-associated galaxy is highlighted in red.
Paper: The Supersonic Project: Star Formation in Early Star Clusters without Dark Matter
Authors: William Lake, Smadar Naoz, Federico Marinacci, Blakesley Burkhart, Mark Vogelsberger, Claire E. Williams, Yeou S. Chiou, Gen Chiaki, Yurina Nakazato, Naoki Yoshida
Figure caption: Plot of the cumulative star formation rate (calculated as total stellar mass divided by time since the start of star formation) in the SIGO as a function of time. Regardless of the time period considered, the star formation rate within the SIGO is the same to within a factor of about 2.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Top: measured background (red points) vs. ETC-predicted values (blue squares). The measured background is the median value of all dithers/exposures. Both backgrounds rise strongly toward longer wavelengths. The measured background is similar to the ETC prediction except at F2100W, where the former is significantly higher. This offset could lead to our measured F2100W depth being shallower than the ETC depth (Section 3.1). For reference, the gray line represents the surface brightness (as measured by the central MIRI pixel) of a simulated massive (﹩\mathrm{log}{M}_{* }/{M}_{\odot }=10.6﹩) star-forming (SFR = 15 M ⊙ yr−1) galaxy at z = 1.2 (Yang et al. 2021). Bottom: relative difference between the measured and ETC backgrounds, i.e., (measured − ETC)/ETC.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Positional differences between MIRI F560W (left) and F1500W (right) sources and their HST counterparts. The dashed circle centers on (0, 0) and has a radius of the MIRI native pixel scale (0.″11). The red plus sign represents the median position of all points. The MIRI sources are detected in the final mosaic. The HST astrometry is aligned to Gaia DR3. We reach an astrometry accuracy of ∼0.″023 (about 0.2 pixels) in F560W and ∼0.″046 (about 0.4 pixels) in F1500W, as labeled.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Illustration of the MIRI imaging in field MIRI1 based on the reduced data products from this work compared to the existing CANDELS WFC3 F160W imaging and Spitzer/MIPS 24 μm imaging. From left to right, the panels show a portion of the imaging from HST F160W, MIRI F770W (blue) + F1000W (green) + F1280W (red), MIRI F1500W (blue) + F1800W (green) + F2100W (red), and MIPS 24 μm. The depth, image quality, and contiguous wavelength coverage from CEERS/MIRI allow us to see a range of MIR “colors” indicative of MIR emission feature redshift through the different MIRI bands.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Comparison of source magnitudes measured in MIRI F560W and F770W vs. IRAC Ch3 and Ch4. The top panels compare MIRI F560W vs. IRAC Ch3, and the bottom panels compare MIRI F770W vs. IRAC Ch4. The red dashed lines indicate the 1:1 (unity) relation. The black vertical lines show the 5σ  detection limits for the IRAC data. The right panels display the difference between the two magnitudes. The red dotted lines indicate the median magnitude difference of the bright sources (IRAC < 23 mag). Red squares represent the median offsets of sources in each magnitude bin, and the error bars represent the median errors of the sources in the bin.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Example of corrupted jumps in one of our F2100W dithers. The left panel displays a group in the raw ramp data, where the data issue happens on the bottom rows of the detector. The right panels display the ramp data (digital number, DN, vs. group) in all of the groups for the two pixels (x–y positions labeled) marked with magenta crosses in the left panel. The dashed vertical line indicates the group displayed in the left panel. The red squares indicate the data affected by the data issue, and all such data are identified and masked out in our reduction. Note that the dips in the last group (group 36 in this example) are discarded by default in stage 1 PIPELINE.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: Comparison of MIRI vs. IRAC filters. The blue/red shaded regions and the blue/red curves indicate MIRI F560W/F770W and IRAC Ch3/Ch4, respectively. The thick black solid curve represents the SED of Arp 256 (Brown et al. 2014), redshifted assuming z = 0.2. The thin black solid and dashed curves represent the SEDs of A0V and K5III stars, respectively.
Paper: CEERS MIRI Imaging: Data Reduction and Quality Assessment
Authors: G. Yang, 光 杨, C. Papovich, M. B. Bagley, H. C. Ferguson, S. L. Finkelstein, A. M. Koekemoer, P. G. Pérez-González, P. Arrabal Haro, L. Bisigello, K. I. Caputi, Y. Cheng, L. Costantin, M. Dickinson, A. Fontana, J. P. Gardner, A. Grazian, N. A. Grogin, S. Harish, B. W. Holwerda, E. Iani, J. S. Kartaltepe, L. J. Kewley, A. Kirkpatrick, D. D. Kocevski, V. Kokorev, J. M. Lotz, R. A. Lucas, R. Navarro-Carrera, L. Pentericci, N Pirzkal, S. Ravindranath, P. Rinaldi, L. Shen, R. S. Somerville, J. R. Trump, A. de la Vega, S. M. Wilkins, L. Y. Aaron Yung
Figure caption: A MIRI1/F770W dither image from the default stage 2 pipeline (left), after our stripe removal (middle), and after our super-background noise subtraction described in Section 2.2.2. The three images are on the same color scale. The noise becomes less prominent after our procedures of stripe removal and super-background.