adsabs/AstroCLIMB huggingface dataset:
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Spatial distributions of electron kinetic energy fluxes in all nine electron-only reconnection events (Events #1–#9). (a)–(i) The ﹩L﹩ component and (j)–(r) the ﹩M﹩ component of electron kinetic energy flux as a function of ﹩{B}_{{L}}﹩. Energy fluxes are scaled by ﹩{E}_{{f}}=\tfrac{{V}_{{\rm{A}}}{B}_{0}^{2}}{{\mu }_{0}}﹩. Events #2–#4 and #6–#8 are asymmetric reconnection. Event #1 exhibits slightly asymmetric number density. Events #1–#8 exhibit a guide field.
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Comparisons between the first and second terms of the electron enthalpy flux. Event #1: (Aa) magnetic field, (Ab) the first term, and (Ac) the second term. Panels (Ba)–(Bc), (Ca)–(Cc), (Da)–(Dc), (Ea)–(Ec), (Fa)–(Fc), (Ga)–(Gc), (Ha)–(Hc), and (Ia)–(Ic) have the same format as panels (Aa)–(Ac) and present the first and second terms of the electron enthalpy flux in Events #2–#9, respectively.
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Spatial distributions of Poynting flux. The ﹩L﹩ component ((a)–(d) and (i)–(m)) and the ﹩M﹩ component ((e)–(h) and (n)–(r)) of Poynting flux as a function of ﹩{B}_{{L}}﹩. Energy fluxes are scaled by ﹩{E}_{{f}}=\tfrac{{V}_{{\rm{A}}}{B}_{0}^{2}}{{\mu }_{{0}}}﹩. Events #2–#4 and #6–#8 are asymmetric reconnection. Event #1 exhibits slightly asymmetric number density. Events #1–#8 exhibit a guide field.
Paper: Energy Flux Densities in Electron-only Magnetic Reconnection in Space Plasma
Authors: Z. Z. Chen, T. Y. Wang, J. Yu, J. Wang, Y. D. Ye, H. S. Fu, J. B. Cao, J. Cui, H. Y. Man, Y. C. Jiang
Figure caption: Electron heat fluxes in Events #2–#8. Event #2: (a) magnetic field and (b) electron heat flux. Panels (Ba)–(Bc), (Ca)–(Cc), (Da)–(Dc), (Ea)–(Ec), (Fa)–(Fc), and (Ga)–(Gc) have the same format as panels (Aa)–(Ab) and present the electron heat flux in Events #3–#8, respectively.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Evolution of the SFR surface density, ΣSFR. Blue points represent individual SFGs, while magenta crosses highlight unresolved sources. Black diamonds show the median ΣSFR in redshift bins, with error bars representing the 1σ error. The solid black line shows the best-fit linear relation, while the lime dashed line shows a comparison from A. Calabrò et al. (2024) for 4 < z < 10.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Evolution of the ratio of the galaxy half-light radius to halo virial radius Re/Rvir for SFGs. The blue data points represent data in this work, with the blue dashed line indicating the median value of the size ratio, Re/Rvir = 2.7% at z ∼ 2−7. The results obtained at lower redshifts are shown with a red square (A. V. Kravtsov 2013), green square (R. S. Somerville et al. 2018), and magenta dashed line (A. V. Kravtsov 2013). The black dashed line shows the theoretical prediction assuming fj = 1; see Equation (6).
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Top: ΣSFR–M* relation across eight redshift bins at z = 2–10. The gray dashed line shows the relation at z ∼ 0 (S. Salim et al. 2023), and magenta and red dashed lines represent the fitting results from A. Calabrò et al. (2024) at 4 < z < 6 and 6 < z < 10, respectively. Bottom: the evolution of ΣSFR in different redshift bins. The fitting results from this work (solid black line) and from A. Calabrò et al. (2024; lime dashed line) are as shown in Figure 11.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: The relation between stellar mass surface density (Σe) and sSFR (﹩{\mathrm{log}}\,\rm{sSFR}\,﹩), with points color coded by Sérsic index nsérsic. The red dashed line marks the threshold ﹩{\mathrm{log}}({\rm{sSFR}})\gt {\mathrm{log}}(0.2/{t}_{{\rm{obs}}})﹩ separating SFGs and QGs. The blue dashed line indicates ﹩{\mathrm{log}}({\rm{sSFR}})\gt {\mathrm{log}}(0.2/{t}_{{\rm{obs}}})+1﹩, with galaxies between the two lines considered to be in a transition phase. Galaxies with nsérsic > 2.5 are considered bulge dominated. The fractions of bulge-dominated galaxies in the star-forming, quiescent, and transition phases are labeled in blue, red, and green, respectively.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Size distribution histograms for SFGs (blue) and QGs (red) in bins of stellar mass and redshift. The distributions are fit with a skewed normal distribution, and the mean size μm, scatter σm, and skewness parameter a are labeled inside each panel.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Surface brightness profile fitting of an example unresolved source at 7 < z < 8. This source is modeled by a Sérsic profile plus a central point-like profile.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: The size–mass relation for SFGs in several bins across a range of redshifts, 2 < z < 10, comparing observations at rest-frame UV and optical wavelengths with results from the cosmological simulations TNG50 (L. Costantin et al. 2023) and THESAN-1 (X. Shen et al. 2024).
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Size difference, ﹩{\rm{\Delta }}{\mathrm{log}}{R}_{e}﹩, of SFGs between the rest-frame optical and UV as a function of stellar mass in different redshift bins at 2 < z < 10. The blue squares and error bars show the median value and its 1σ distribution. The dark dashed lines indicate the reference line ﹩{\rm{\Delta }}{\mathrm{log}}{R}_{e}=0﹩.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Evolution of the modeled mean size, μm, in different mass bins. Fitting results for SFGs in the form of ﹩{\mu }_{m}\propto {(1+z)}^{{\beta }_{m}}﹩ are shown by dashed lines.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Top: the evolution of rest-frame optical sizes for SFGs (blue circles) and QGs (red circles) at a fixed stellar mass 5 × 1010M⊙ at 2 < z < 10, with comparisons to previous studies. The fitting results for SFGs and QGs are shown by the blue and red solid lines, respectively, corresponding to Re ∝ (1 + z)−1.21±0.05 and Re ∝ (1 + z)−0.81±0.26, with the shaded regions representing the 1σ uncertainties. Utilizing recent JWST data, the results of SFGs from K. Ormerod et al. (2024), R. G. Varadaraj et al. (2024), E. Ward et al. (2024), T. Morishita et al. (2024), and N. Allen et al. (2025) are illustrated by brown, cyan, magenta, orange, and green colors, respectively. Lime pentagons display results for QGs (K. Ito et al. 2024). The dark blue and dark red represent HST results of SFGs and QGs, respectively, from A. van der Wel et al. (2014). Bottom: the evolution of the slope α (left) and intrinsic scatter ﹩{\sigma }_{{\mathrm{log}}{\,{\rm{R}}\,}_{{e}}}﹩ (right), with colors the same as in the top panel.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: The rest-frame optical size–mass distribution of SFGs (blue) and QGs (red) presented in redshift bins at 2 < z < 10. The black solid lines indicate the best-fit size–mass relation of SFGs and QGs (see also Table 1). The thick black and lime dashed lines show the fitting results at 2 < z < 3 in this work and z ∼ 2.75 obtained by A. van der Wel et al. (2014), respectively. The horizontal black dotted line in each panel indicates the PSF size (FWHM/2) of the filter that is closest to the rest-frame optical in each redshift bin. The numbers of galaxy data points are labeled in the lower-left corner in each redshift bin.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: Rest-frame NUV − r − J color–color diagram for galaxies at 2 < z < 10. Data points are color coded according to their sSFR. The magenta line indicates the NUV − r − J criteria (see Equation (1)), separating QGs (top left) from SFGs (bottom right). Additionally, galaxies are required to meet the sSFR criterion, e.g., ﹩{\mathrm{log}}({\rm{sSFR}})\lt {\mathrm{log}}(0.2/{t}_{{\rm{obs}}})﹩ for QGs, where tobs is the observed Universe age. In each panel, the numbers of QGs and SFGs classified using the color–color diagram are labeled in black, while those further classified with the additional sSFR criterion are labeled in blue and red inside the bracket.
Paper: COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10
Authors: Lilan Yang, Jeyhan S. Kartaltepe, Maximilien Franco, Xuheng Ding, Mark J. Achenbach, Rafael C. Arango-Toro, Caitlin M. Casey, Nicole E. Drakos, Andreas L. Faisst, Steven Gillman, Ghassem Gozaliasl, Marc Huertas-Company, Shuowen Jin, Daizhong Liu, Georgios Magdis, Richard Massey, John D. Silverman, Takumi S. Tanaka, Si-Yue Yu, Hollis B. Akins, Natalie Allen, Olivier Ilbert, Anton M. Koekemoer, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft
Figure caption: The rest-frame wavelength probed by each of the COSMOS-Web filters as a function of redshift. The shaded background purple (red) regions indicate the rest-frame UV (optical) range, i.e., 2000–4000 Å  (4000–6000 Å) for UV (optical). For example, at 6 < z < 10, the F277W (F444W) filter probes the rest-frame UV (optical) properties of galaxies.
Paper: A Neural-network Model for Quickly Solving Multiple-band Light Curves of Contact Binaries
Authors: Kai Li, Li-Heng Wang, Xiang Gao
Figure caption: The structure of the network.
Paper: A Neural-network Model for Quickly Solving Multiple-band Light Curves of Contact Binaries
Authors: Kai Li, Li-Heng Wang, Xiang Gao
Figure caption: The distribution of the difference between the physical parameters obtained.
Paper: A Neural-network Model for Quickly Solving Multiple-band Light Curves of Contact Binaries
Authors: Kai Li, Li-Heng Wang, Xiang Gao
Figure caption: The fitted LCs of the eight targets.
Paper: A Neural-network Model for Quickly Solving Multiple-band Light Curves of Contact Binaries
Authors: Kai Li, Li-Heng Wang, Xiang Gao
Figure caption: The posterior parameter distributions and the best-fit model for an example system.
Paper: The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey
Authors: Brendan P. Crill, Yoonsoo P. Bach, Sean A. Bryan, Jean Choppin de Janvry, Ari J. Cukierman, C. Darren Dowell, Spencer W. Everett, Candice Fazar, Tatiana Goldina, Zhaoyu Huai, Howard Hui, Woong-Seob Jeong, Jae Hwan Kang, Phillip M. Korngut, Jae Joon Lee, Daniel C. Masters, Chi H. Nguyen, Jeonghyun Pyo, Teresa Symons, Volker Tolls, Yujin Yang, Michael Zemcov, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Tzu-Ching Chang, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Andreas L. Faisst, Richard M. Feder, Michael W. Werner
Figure caption: Example simulated exposure images near the north ecliptic pole. In each image, the wavelength increases in the downward direction (see Table 2). The short-wavelength bands 1, 2, and 3 are in the top row, and the midwavelength bands 4, 5, and 6 are in the bottom row. The pointings are approximately equivalent for the two focal planes. The most prominent components are stars, ZL, and DGL. The ZL is spatially smooth with a steeply rising spectral energy distribution at long wavelengths (see Table 2 for the wavelength coverage of each band); this creates a strong vertical gradient in the LVF images for the longest wavelengths. The DGL manifests as nebular anisotropies that are visible in the shorter-wavelength arrays. Below the midpoint of the band 4 image, the horizontal band is due to a polycyclic aromatic hydrocarbon emission feature at 3.3 μm. At the bottom of band 3 and the top of band 4, there is a dimming due to the minimum in the optical efficiency of the dichroic beam splitter.
Paper: The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey
Authors: Brendan P. Crill, Yoonsoo P. Bach, Sean A. Bryan, Jean Choppin de Janvry, Ari J. Cukierman, C. Darren Dowell, Spencer W. Everett, Candice Fazar, Tatiana Goldina, Zhaoyu Huai, Howard Hui, Woong-Seob Jeong, Jae Hwan Kang, Phillip M. Korngut, Jae Joon Lee, Daniel C. Masters, Chi H. Nguyen, Jeonghyun Pyo, Teresa Symons, Volker Tolls, Yujin Yang, Michael Zemcov, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Tzu-Ching Chang, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Andreas L. Faisst, Richard M. Feder, Michael W. Werner
Figure caption: Observation wavelengths vs. time (in days since the start of the mission) using the QuickCatalog for a primary calibration source (GD71) in one mission year. The survey plan covers this particular source in two distinct epochs in this year, and is representative of the coverage of most sources away from the ecliptic pole regions.
Paper: The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey
Authors: Brendan P. Crill, Yoonsoo P. Bach, Sean A. Bryan, Jean Choppin de Janvry, Ari J. Cukierman, C. Darren Dowell, Spencer W. Everett, Candice Fazar, Tatiana Goldina, Zhaoyu Huai, Howard Hui, Woong-Seob Jeong, Jae Hwan Kang, Phillip M. Korngut, Jae Joon Lee, Daniel C. Masters, Chi H. Nguyen, Jeonghyun Pyo, Teresa Symons, Volker Tolls, Yujin Yang, Michael Zemcov, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Tzu-Ching Chang, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Andreas L. Faisst, Richard M. Feder, Michael W. Werner
Figure caption: SPHEREx Simulator architecture.
Paper: The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey
Authors: Brendan P. Crill, Yoonsoo P. Bach, Sean A. Bryan, Jean Choppin de Janvry, Ari J. Cukierman, C. Darren Dowell, Spencer W. Everett, Candice Fazar, Tatiana Goldina, Zhaoyu Huai, Howard Hui, Woong-Seob Jeong, Jae Hwan Kang, Phillip M. Korngut, Jae Joon Lee, Daniel C. Masters, Chi H. Nguyen, Jeonghyun Pyo, Teresa Symons, Volker Tolls, Yujin Yang, Michael Zemcov, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Tzu-Ching Chang, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Andreas L. Faisst, Richard M. Feder, Michael W. Werner
Figure caption: “Rogues’ gallery” of various local and instrumental features modeled by the Simulator. These images are drawn from a variety of bands and sky positions and are meant to show typical examples of each effect. The photocurrent scaling varies between images, but typically covers a range of about 1 e− s−1. (A) An example of a signal expected from an Earth satellite crossing the SPHEREx field of view. This 100 × 100 pixel cutout captures a small part of a streak that crosses the entire detector. (B) Electrical crosstalk, where the primary source—a bright star to the left—is marked with an “x,” and the first three electrical crosstalk images are circled. We have exaggerated the effect by 25× in amplitude to highlight its structure. (C) Flat-field imperfections due to detector artifacts, with some examples circled. The simulated images include responsivity variations that, in addition to large-scale structures, can cause localized regions of poor photoresponse that are modeled by the Simulator. (D) Frame-edge ghost, which is due to light from bright stars just off the image to scatter off the frame that holds the filter above the detector array. This causes roughly linear features perpendicular to the edge of the image. (E) Diffuse beam-splitter ghosts caused by internal reflections in the optical system. These are large circular features (centered on the “+” marks) that are sourced by bright stars in certain geometries compared with the focal plane. (F) Detector image persistence, an electrical effect where the charge caused by the images of bright sources is not fully flushed from the detector material after a well reset. The circled source is spurious and was caused by a bright star in a previous exposure whose image has not been fully erased by the reset. These images look similar to stars and decay away with a time constant of several hundred seconds.
Paper: The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey
Authors: Brendan P. Crill, Yoonsoo P. Bach, Sean A. Bryan, Jean Choppin de Janvry, Ari J. Cukierman, C. Darren Dowell, Spencer W. Everett, Candice Fazar, Tatiana Goldina, Zhaoyu Huai, Howard Hui, Woong-Seob Jeong, Jae Hwan Kang, Phillip M. Korngut, Jae Joon Lee, Daniel C. Masters, Chi H. Nguyen, Jeonghyun Pyo, Teresa Symons, Volker Tolls, Yujin Yang, Michael Zemcov, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Tzu-Ching Chang, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Andreas L. Faisst, Richard M. Feder, Michael W. Werner
Figure caption: Separated simulation components for array 1 for the exposure image shown in Figure 2. The component images can be simulated independently and then summed linearly to produce the full image. Individually resolved galaxies can be included in simulation of the extragalactic background light, or, to simulate the true sky, galaxies can be instead drawn from the reference catalog. Photon noise is calculated from all optical components. Read noise and dark current are estimated from prelaunch laboratory testing.