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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: SEDs of the ZL and DGL used in the Simulator. The gray color scale referenced to the left-hand axis shows the surface brightness density computed over 256 random draws from the modified Kelsall ZL model covering the entire two-year survey. There is a factor of ∼3 brightness variation between the ecliptic plane and the poles, with smaller variations at longer wavelengths. The red line for DGL referenced by the scale on the right-hand axis shows the conversion factor νbν used to convert the far-infrared brightness to surface brightness in the near-infrared (K. Sano et al. 2016). The conversion is brightest at optical wavelengths and shows a broad feature between 3 and 3.5 μm due to polycyclic aromatic hydrocarbons in the ISM. At high galactic latitudes, the far-infrared emission typically has brightness ∼1 MJy sr−1 in these units, which multiplying by νbν leads to a signal that is typically ∼10 nW m−2 sr−1 in the near-infrared. This is over an order of magnitude fainter than the ZL.
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: Split PSFs for the central detector pixel of band 3. The core PSF is defined over a much smaller solid angle and is stored at finer resolution. The extended PSF is stored over an area that is equal in size to the detector’s field of view (∼3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 × 3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5); for this figure, we have truncated to the central ﹩4^{\prime} \rm{}\,\rm{}\,\times 4^{\prime} \rm{}\,\rm{}\,﹩. The core-PSF simulations are tapered in their outer radii, and the extended-PSF simulations are tapered in their inner radii. The two are consistently normalized. The split PSFs can be convolved separately, and the resulting images can be summed to simulate the effect of the full PSF (as in Figure 10).
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: Simulated maps of EBL. These are used as inputs to the Simulator. The native resolution of these maps is 1″. To better visualize the large-scale structure, we have here smoothed the maps to 1′. A full simulation set typically contains more than 100 maps in order to sample the SPHEREx wavelength range at the spectral resolution of the instrument. We have here selected a smaller sample of representative wavelengths. The above maps cover an area of 3° × 3° near the north ecliptic pole, which is the center of one of SPHEREx’s deep fields. The simulated maps can be constructed over larger areas and translated to any region of sky. These simulations are accompanied by galaxy catalogs with simulated photometry to emulate the SPHEREx reference catalog.
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: Simulated images of extended sources observed with band 5. These images include all of the components from Figure 5 with the addition of extended sources drawn from the WISE Extended Source Catalog. Because these example objects are relatively bright, the background is dominated by stars and ZL, where the latter produces a prominent vertical gradient in LVF images. The black dotted grid corresponds to ecliptic coordinates while the white dotted grid corresponds to International Celestial Reference System coordinates.
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: Thumbnail of the star component for band 1 for the pointing shown in Figure 2. Notice the extended-PSF halos. This image is produced by convolving the star catalog with the core PSF and separately convolving with the extended PSF (Figure 11). The two convolved images are then summed to simulate the effect of the full PSF.
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: Panel of PSFs at evenly spaced focal-plane positions in band 3. Notice that the PSF varies continuously in both directions across the band. In the downward direction, the PSFs generally widen due to an increasing wavelength; in the horizontal direction, the variation is mainly due to a defocusing of the telescope optics. The underlying optical simulations provide PSFs at discrete locations, and the Simulator can interpolate among those locations.
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: An example of simulated source photometry using QuickCatalog for a primary calibration source (GD71). Upper panel: simulated primary photometry (at the exact wavelength observed by SPHEREx). Lower panel: the secondary catalog, containing photometry binned into 102 spectral channels (blue) and synthetic photometry (orange squares) where SPHEREx photometry data are binned into synthetic photometry for LSST, 2MASS, and WISE bands.
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: The Simulator bandpass model for the shortwave detectors 1, 2, and 3 (top, middle, and bottom rows, respectively). Left column: the band center wavelength λ0 as a function of position on the array with boundaries of the spectral channels indicated and labeled with the mean wavelength. Right column: bandpass response functions (normalized to peak response) for pixel locations in the center of each spectral channel. The slight curvature is an effect known as “smile” that is due to the LVF manufacturing process. The region of the detector outside of any spectral channel will also be present in the spectral image but is not included in the spectral coverage of the survey.
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: The Simulator bandpass models for the midwave detectors 4, 5, and 6 (top, middle, and bottom rows, respectively). Left column: the band center wavelength λ0 as a function of position on the array with boundaries of the spectral channels indicated and labeled with the mean wavelength. Right column: bandpass response functions (normalized to peak response) for pixel locations in the center of each spectral channel.
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 5σ point source sensitivity in a single visit (with the prelaunch integration time 112.5 s) vs. wavelength as estimated by the Simulator; colors represent bins of ecliptic latitude β.
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: Predicted SPHEREx 5σ point source sensitivity in a single visit as a function of the local background surface brightness, which, when dominated by zodi, depends on time of year and line-of-sight direction. The domain of the curves shows the range of zodi background expected for each detector during the two-year SPHEREx survey, with the thicker line spanning the fifth to 95th percentiles.
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: An example readout noise realization for detector 2. Left: per-pixel noise. Right: per-pixel plus correlated readout channel noise. Noise is realized for each simulated exposure and summed into the output image as an additive term.
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: Dark current templates used in the Simulator. The images in the top row are the shortwave detectors 1, 2, and 3, and those in the bottom row are the midwave detectors 4, 5, and 6. These templates are used to generate random draws of dark current for each simulated exposure.
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: An example of inserting compact sources with detector 2. Left: source flux is introduced as delta functions in an oversampled high-resolution image. Center: the high-resolution image is convolved with the core PSF model. Right: finally, the image is rebinned to SPHEREx native resolution. The grid lines show SPHEREx detector pixel edges.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Comparison between GBS3 stellar parameters and properties estimated from TRES spectra using uberMS in TP mode (A), uberMS in MS mode (B), and SPC (C). In each set of subplots, the upper row shows dwarf stars (here approximated by logg > 4 dex), while the lower row shows evolved stars (logg < 4 dex). Note that error bars are only plotted for GBS3 values, not for our measurements. The dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: The metallicities and effective temperatures estimated from TRES spectra of 67 Hyades dwarf stars. From left to right, the panels show the results from uberMS in TP mode (no isochrones), uberMS in MS mode (including isochrones), and SPC. Points are color coded based on stellar mass, as calculated from a Hyades-specific Ks-band mass–luminosity relation. Black dotted lines represent sixth-order Legendre polynomial fits to the data, with coefficients given in Table 1.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: In the upper panels, we show a comparison between APOGEE [Si/Fe] and [Mg/Fe] abundance ratios and the [α/Fe] ratio we estimate from uberMS in MS mode using TRES data. The lower panels compare SPOCS [Si/Fe] and [Ti/Fe] with our uberMS estimates; HD 82558 and HD 80133 have been neglected from this plot due to their potentially erroneous values (see the text). The dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Our same uberMS analysis from panel B of Figure 2, but compared to the iron abundance and alpha enrichments for the GBS3 sample measured in L. Casamiquela et al. (2025). The dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Comparison between SPOCS stellar parameters and properties estimated from TRES spectra using uberMS in TP mode (A), uberMS in MS mode (B), and SPC (C). In each set of subplots, the upper row shows dwarf stars (here approximated by logg > 4 dex), while the lower row shows evolved stars (logg < 4 dex). The dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Comparison between APOGEE stellar parameters and properties estimated from TRES spectra using uberMS in TP mode (A), uberMS in MS mode (B), and SPC (C). In each set of subplots, the upper row shows dwarf stars (here approximated by logg > 4 dex), while the lower row shows evolved stars (logg < 4 dex). Note that error bars are only plotted for APOGEE values, not for our measurements. The dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Comparison between properties estimated from TRES spectra. The upper panel A(B) compares the two uberMS modes, while the lower panel (B)C compares MS mode to SPC. In each set of subplots, the upper row shows dwarf stars (here approximated by logg > 4 dex), while the lower row shows evolved stars (logg < 4 dex). The dashed lines indicate unity. Note that in the upper panel, we use ﹩{\rm{\Delta }}{\mathrm{log}}g﹩ as the color bar for the [Fe/H] residual plots instead of Teff: since the main difference between the modes is the constraint on ﹩{\mathrm{log}}g﹩ from the isochrone prior, we are unsurprised to find that the differences between the modes’ [Fe/H] estimates are correlated with ﹩{\rm{\Delta }}{\mathrm{log}}g﹩.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: uberMS in MS mode applied to TRES data of the components of 18 wide binaries. Dashed lines indicate unity. The upper panels compare the [Fe/H] (left) and [α/Fe] (right) estimates for the primary and secondary. The lower panel shows how the difference in [Fe/H] estimates varies with the effective temperature of the secondary: we observe a similar systematic offset as was seen in the Hyades data, where uberMS underestimates [Fe/H] for mid-to-late K dwarfs.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: The same MS-mode uberMS vs. SPOCS comparison as panel (B) of Figure 6, but replacing the J. A. Valenti & D. A. Fischer (2005) SPOCS parameters with the revised parameters from J. M. Brewer et al. (2016). Some stars were not analyzed in J. M. Brewer et al. (2016) and hence are omitted. Dashed lines indicate unity.
Paper: Metallicities from High-resolution TRES Spectra with uberMS: Performance Benchmarks and Literature Comparison
Authors: Emily K. Pass, Phillip A. Cargile, Victoria DiTomasso, Romy Rodríguez Martínez, David Charbonneau, David W. Latham, Andrew Vanderburg, Allyson Bieryla, Samuel N. Quinn, Lars A. Buchhave
Figure caption: Results from uberMS in MS mode for TRES data of asteroids. Dashed lines indicate solar values. The black points represent each individual asteroid spectrum, while the cyan cross is a coadded spectrum of all observations of all asteroids.