adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: TSM, as defined in Kempton et al. (2018), for TOIs in multiplanet systems around bright M dwarfs (T eff < 4000 K and T mag < 11.5) with R  p  < 4 R ⊕ as of 2022 July 7. TIC stars are sorted in decreasing order of second largest TSM value in the system. Color corresponds to host T mag and size corresponds to planet radius. The gray dashed line is the atmospheric follow-up threshold recommended by Guerrero et al. (2021) for sub-Neptunes. TOI 4342 is among the top 10 systems with multiple planets that are well suited for atmospheric characterization.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: Difference images for TOI 4342 b and TOI 4342 c, made using 20 × 20 pixel cutouts of the Sector 27 TESS FFIs (top). A close-up of the central 5 × 5 pixels is also shown (bottom). The third column shows the average of out-of-transit images, which should represent a direct image of the field near the target star. The target TIC 354944123 is indicated with a pink star, while nearby stars down to ΔT = 4 mag are plotted as white circles with sizes scaled by brightness. The difference images for both planet candidates indicate the transit sources are collocated with the target star. The color bars are all in units of electrons per second.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: Top: detrended TESS light curve in gray, binned values in purple, with transits highlighted for each TOI 4342 b (blue) and TOI 4342 c (orange). Middle: TESS and LCOGT light curves folded on the best-fit period and epoch found in Section 3.2.1. Different background-subtracted observations are shown in different colors for each transit with the best-fit model in black. Bottom: residual flux between the fully combined light curve and the model.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: Insolation and orbital period vs. planet size. TOI 4342 b and TOI 4342 c are shown in cyan over occurrence contours for host stars with M * < 0.97 M ⊙ from Fulton & Petigura (2018). M-dwarf TOIs as of 2022 July 7 are plotted as well, with multiplanet system planets highlighted in magenta. TOI 4342 b and TOI 4342 c both lie in the upper end of the radius valley.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: Top: SPOC SAP light curve with our correction trend (described in Section 2.1) in blue. This trend, formed from quaternion data and basis splines to remove systematics and long-timescale variability, is divided out of the raw light curve to create our final flattened light curve. Bottom: Lomb–Scargle periodograms of the SAP SPOC light curve for each sector of observation. We see peaks around 14 days marking stellar variability, but we cannot pin down a specific period due to the large gap between observations.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: Gemini South Zorro speckle imaging 5σ contrast curve (full plot) and reconstructed images (inset plot) in the 832 nm band. The diffraction limit of the instrument is 20 mas.
Paper: TESS Discovery of Twin Planets near 2:1 Resonance around Early M Dwarf TOI 4342
Authors: Evan Tey, Chelsea X. Huang, Michelle Kunimoto, Andrew Vanderburg, Avi Shporer, Samuel N. Quinn, George Zhou, Karen A. Collins, Kevin I. Collins, Eric L. N. Jensen, Richard P. Schwarz, Ramotholo Sefako, Tianjun Gan, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Kathryn V. Lester, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, George R. Ricker, Roland K. Vanderspek, David W. Latham, S. Seager, Jon M. Jenkins, Joshua N. Winn, Douglas A. Caldwell, David Charbonneau, Christopher J. Burke, Zahra Essack
Figure caption: SOAR speckle autocorrelation function (inset plot) and its 5σ detection sensitivity curve (main plot) in the Cousins I band.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: The eccentricity distribution of our widened binaries compared to the known distribution of both tight and ultrawide binaries. Also plotted for comparison is a thermalized eccentricity distribution.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: The inclinations of our simulated binaries that have become ultrawide vs. those that have not. These are compared to the inclinations of observed ultrawide binaries and tight binaries.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: Color–magnitude diagrams of ZAMS Population III stars in the most optimal JWST bands listed in Table 2 at four different redshifts. Synthetic photometry is shown for both detailed opacity calculations based on model atmospheres and the corresponding blackbody profiles. Selected initial stellar masses are indicated in both cases with red and blue markers, respectively. The red markers are labeled in solar masses. The blue markers correspond to the same masses as the red markers in the same order along the color–magnitude curve. Observability limits for the JWST are shown in gray and labeled with the required gravitational lensing magnification, μ.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: Mass–magnitude relationships for ZAMS Population III stars in the most optimal JWST bands listed in Table 2 at four different redshifts, color coded. Note that a different band is used at each redshift. The equivalent relationships for the corresponding blackbody profiles are shown in dashed lines for comparison. The observability limits for the JWST are indicated with black markers for each relationship shown. The displayed observability limits are grouped by the required gravitational lensing magnitification, μ.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: The 5th and the 95th percentiles of the wavelength distribution of the source function at a range of Rosseland mean optical depths for the solar atmosphere (bottom) and a near-Eddington Population III atmosphere with M = 820.2 M ⊙ (top). The cases of the exact solution for the source function and the LTE approximation are shown in solid red and dashed black, respectively. The optical depth where the gas temperature matches the effective temperature of the star is highlighted for reference. The background color scheme corresponds to the total atmospheric opacity as a function of both the wavelength and Rosseland optical depth. The discontinuous changes in opacity are due to bound–free absorption breaks.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: Synthetic spectra of ZAMS Population III stars for initial stellar masses between 1 M ⊙ and the Eddington limit (820.2 M ⊙). For clarity, each spectrum is shown on a separate color-coded vertical scale. The blackbody spectra at the corresponding effective temperatures are shown in dashes for reference. Important bound–free absorption breaks are highlighted with vertical lines and labeled.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: Surface parameters of ZAMS Population III stars compared to the exact calculation of the Eddington limit, including non-LTE effects and nongray atmospheric opacity. The dashed curve traces out an alternative locus of surface parameters in the absence of the CNO break in the mass–radius relationship at ﹩{M}_{\mathrm{bp}}^{(R)}\approx 16\ {M}_{\odot }﹩. The surface parameters extracted directly from selected MESA models are shown with red markers and labeled by the initial masses (in M ⊙). The maximum stellar mass with a convergent ATLAS atmosphere is shown with the blue circle at 820.2 M ⊙. The “classical” (gray atmosphere, LTE) Eddington limit from Equation (8) is shown for reference. Note that the exact Eddington limit results in a lower maximum mass value.
Paper: Characterization of Population III Stars with Stellar Atmosphere and Evolutionary Modeling and Predictions of their Observability with the JWST
Authors: Mikaela M. Larkin, Roman Gerasimov, Adam J. Burgasser
Figure caption: Mass–radius relationship from the metal-free evolutionary models calculated in this study alongside the best-fit power-law approximation given in Equation (1) and using the best-fit parameters in Table 1. Equivalent relationships for nonzero metallicities were calculated as well and are shown with dashed lines for comparison. Each dashed curve is parameterized by the total metal mass fraction, Z. The vertical line indicates the break in the best-fit power-law relationship that originates from the onset of the CNO cycle in the core. The point where the energy production rates of the proton–proton chain (L pp) and the CNO cycle (L CNO) match is indicated with blue squares for every mass–radius relationship shown.
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: Locations of YSO groups (green circles) and isolated YSOs with spectra (magenta stars) plotted on the Vergely et al. (2022) extinction map (gray scale). The map uses a heliocentric Galactic (x,y) coordinate system, with the Sun at (0, 0) (blue symbol), the Galactic center on the positive x-axis, and the direction of rotation at the location of the Sun parallel to the y-axis. Dashed magenta lines indicate the boundaries (in Galactic longitude) of the area from which the program stars were selected.
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: Left: equivalent width of the 5780 Å DIB vs. A  V  values from SED fitting. The lines indicate relations from Vos et al. (2011), for “σ-type” sightlines, and from Carvalho & Hillenbrand (2022), for “ζ-type” sightlines. Sources with W λ (5780)/W λ (5797) > 3.3 (indicative of σ-type sightlines) are red. Right: extinctions along the line of sight to each program star from the Green et al. (2019) Galactic dust map. The ordinate shows extinctions at the stars’ distance moduli (DM) −0.2 and + 0.2, and the abscissa is the extinction of the star itself. The black, dashed line marks equal A  V  values.
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: Line profiles for program stars with clear Hα emission. The observed spectra are shown in magenta, and the corresponding templates are shown in black. Spectra are plotted in continuum units, as indicated by the blue scale bar.(The data used to create this figure are available.)
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: Comparison of the photometric and astrometric properties of the program stars (red points) observed with Palomar/DBSP to the full SPICY catalog (green points). Left: near-infrared H − K vs. Spitzer/IRAC [4.5]–[8.0] color–color diagram. Center: Gaia G-band magnitude vs. G − G RP. Right: Gaia parallax vs. parallax error (log scale). The black lines indicate the cuts used for selecting stars for follow-up.
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: Representative section of the GLIMPSE survey area (boundary shown in black) containing two of the program stars (red circles). Other SPICY stars are indicated by the green points. Young stellar groups from Paper I, supplemented by groups from Cantat-Gaudin et al. (2020) and Kounkel et al. (2020), are indicated by the black X’s.
Paper: Spectroscopic Confirmation of a Population of Isolated, Intermediate-mass Young Stellar Objects
Authors: Michael A. Kuhn, Ramzi Saber, Matthew S. Povich, Rafael S. de Souza, Alberto Krone-Martins, Emille E. O. Ishida, Catherine Zucker, Robert A. Benjamin, Lynne A. Hillenbrand, Alfred Castro-Ginard, Xingyu Zhou
Figure caption: HR diagram for the observed SPICY stars. PARSEC isochrones are drawn at 0.3, 1, 3, 10, and 30 Myr. Stars with Hα emission are color coded magenta.
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: Targeting accuracy for DESI fiber robots over a 3 month period of survey operations in fall 2021, during which the Focal Plane System acquired more than 7.8 million targets. The shallower red histogram shows “blind” move accuracy, i.e., the first open-loop move made toward each target. The sharper blue histogram shows positioning error after a single correction move, based on feedback from the FVC (Section 2.5). Blind move rms error is 54 μm, with 0.35% of attempted targets having error >200 μm. After the correction move, the rms error is 9 μm, with 0.03% outliers >200 μm. Errors here are with respect to the commanded target positions, and include significant contributions of measurement noise (Section 6.6) due to centroiding precision limits (∼3 μm) and air turbulence in the dome (∼3–8 μm). Turbulence subtraction code introduced in late 2021 further reduced the error to 6 μm rms. Figure 5
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: Distributions for several key calibration parameters for the fiber positioner robots. At left are the kinematic arm lengths of the two robot axes. “R1” is the distance from the θ rotation axis to the ϕ rotation axis. “R2” is the distance from the ϕ axis to the fiber. The maximum radius to which a given robot unit can move its fiber is its particular value for (R1 + R2). At the center of each unit there is an inaccessible zone of radius ∣R1 − R2∣. The middle and right plots show the maximum travel ranges from hardstop-to-hardstop for the θ and ϕ axes, respectively. The ϕ range distribution is bimodal due to a period of several months during robot production where ϕ bearings were being glued at a spacing ∼0.5 mm further than nominal off their housings, thus increasing the effective travel range. Other calibration parameters (not shown here) include the center position of the θ rotation axis, angular zero-points of θ and ϕ, and effective gear output ratio for each axis (equal to 1.0 for nominally functioning robots).