adsabs/AstroCLIMB huggingface dataset:
Paper: Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection
Authors: X. Cheng, C. Xing, G. Aulanier, S. K. Solanki, H. Peter, M. D. Ding
Figure caption: a1–a3) Time sequence of composite of the AIA 131 Å (red) and 211 Å (cyan) difference images showing the early rise and eruption of the pre-eruptive MFR and induced flare. b1–b3) The AIA 1600 Å images display the flare ribbons, and the field of view is indicated by the box in panel a1. c1–c3) The EUVI 195 Å difference images (subtracting the image at 14:00 UT) represent the dimming regions, which include the footpoints of the erupting MFR. The left footpoint (L) is indicated in panel a1, and the left dimming (ED) and right two dimmings (DR1 and DR2) are pointed out by the arrows in panel c1.
Paper: Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection
Authors: X. Cheng, C. Xing, G. Aulanier, S. K. Solanki, H. Peter, M. D. Ding
Figure caption: X-ray emission and spectra. a) RHESSI X-ray source in the energy ranges of 3–6 keV (blue), 6–12 keV (red), and 12–25 keV (yellow) overlaid on the AIA 131 Å difference images (subtracting the image taken at 15:50 UT) showing the energy release locations by precursor reconnection. The two contours for each energy band denote 50% and 80% of their maximum emissions. The image on the left and right is scaled linearly and logarithmically, respectively. b) Spectra of X-ray emission and their temporal evolution. The curves in blue display the best fitting to background-subtracted spectra (curves in gray), with the ones in red and yellow indicating the thermal and nonthermal thin-target model, respectively. The resulting fitting residuals are shown in the bottom panels.
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: The average UV luminosity for 1010–1011 M ⊙ haloes as a function of redshift derived from abundance matching (solid blue line), with its associated uncertainty (shaded blue band). The best-fitting evolution of the average relation (Equation (2)) is indicated by the purple dotted line. Overplotted are the expected fractions of Population III stars (averaged over all haloes) and that of pristine gas (with an arbitrary normalization) from the results of Furlanetto & Loeb (2005), Sun et al. (2021) and the gas accretion rate, proportional to (1 + z)5/2 (Furlanetto & Mirocha 2022). The red dashed lines indicate the range of increase in UV luminosity from a top-heavy IMF consisting of 300–1000 M ⊙ stars (Bromm et al. 2001).
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Modified (solid, Equation (5)) and original (dashed) halo abundances over z ∼ 9–16 resulting from the modification to the transfer function, Equation (4).
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Top panel: original and modified forms of the transfer function used in computing the power spectrum for halo abundances. Lower panel: ratio of the modified and original transfer functions in the relevant k-range. The region enclosed by 1 < k/(Mpc−1) < 10 is shown by the dashed lines.
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Spectral energy density of AGN in the 0.5–7 keV band corresponding to the observed average UV luminosity at various redshifts, compared to a fiducial AGN spectrum at z ∼ 6 normalized to ﹩{\mathrm{log}}_{10}(\nu {L}_{\nu }/\mathrm{erg}\,{{\rm{s}}}^{-1})﹩ (4500 Å) = 45.5 (Shen et al. 2020).
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: Evolution of UV luminosity in 1010–1011 M ⊙ haloes as a function of redshift corresponding to the modified cosmological power spectrum. The best-fitting (constant) value is shown by the dotted purple line.
Paper: Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf
Authors: Joanne L Pledger, Michael M Shara
Figure caption: Hubble Space Telescope ACS/WFC images of the ∼2 arcsec2 region around the site of SN 2023ixf in F435W (top left), F555W (top right), and F814W (bottom) filters. The location of the two sources identified in the F814W image are marked with a circle (with the size corresponding to 1σ positional error), while the SN location is indicated by a cross. We note that north is up and east is left.
Paper: Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf
Authors: Joanne L Pledger, Michael M Shara
Figure caption: HST/ACS F814W image taken in 2002 November (left) and Gemini/GMOS r-band image taken in 2023 June (right) at the site of SN 2023ixf in M101, which became available after the initial submission of this Letter. The location of the SN is highlighted and is coincident with a single source in the F814W image. We note the SN is on the edge of one of the GMOS-N chips.
Paper: Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf
Authors: Joanne L Pledger, Michael M Shara
Figure caption: Mean x-profile of the source at the location of SN 2023ixf (dashed line), and for comparison the mean x-profile of a nearby pointlike star (solid line). The peak at x ∼ 5 corresponds to the brightest part of the source, and another peak is suggested at x ∼ 3 for the second, fainter source that is not seen in the comparison star.
Paper: Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum
Authors: Hamsa Padmanabhan, Abraham Loeb
Figure caption: The average UV luminosity as a function of redshift and halo mass from the JWST observations (solid lines) with the shaded bands denoting the uncertainties inferred from the UV LFs. Also plotted are the predicted luminosity–halo mass relations from the simulations of (Kannan et al. 2023, dashed blue line) and the empirical findings at lower redshift (Mashian et al. 2015, orange dotted line).
Paper: Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
Authors: J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui
Figure caption: Left: orbital modulation of ASJ2055 as observed by ZTF (λ = 750 nm). The solid line is the model light curve (Section 3.3). Right: spectrum of ASJ2055. The solid line and dashed line are Koester’s WD model (Koester 2010) and the Planck function, respectively, with the effective temperature of T eff,wd = 80,000 K, where the radius of the WD and the distance to the target from Earth are assumed to be R WD = 1.7 × 109 cm and d = 1.7 kpc, respectively. The dashed–dotted lines represent theoretical spectra of the heated companion star (Section 3.3) at the optical peak (ϕ orb = 0) and minimum (ϕ orb = 0.5), respectively. For the observed data, the interstellar dust extinction is calculated using the model of Fitzpatrick & Massa (2007; R  V  = 3.1), implemented in the Python code extinction (Barbary 2016); the extinction in the V bands, A  V  = 0.5, is estimated from the relation N H/A  V  ∼ 1.8 × 1021 cm2 mag−1, with N H ∼ 9 × 1020 cm2 inferred from the sky position of ASJ2055 (https://heasarc.gsfc.nasa.gov/cgi-bin/Tools/w3nh/w3nh.pl). The error bars of each observational point are smaller than the size of each symbol.
Paper: Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
Authors: J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui
Figure caption: Top panels: TESS-PDCSAP flux for AJ2055 taken in 2021 July/August (left) and 2022 August (right), downloaded from MAST. Bottom panels: the LS periodograms of the 2021 (left) and 2022 (right) TESS data after subtracting the mean value of the light curve. The frequency range of 75–250 days−1 is displayed to present the signals of f 0 ∼ 147 days−1 and f 1 ∼ 192 days−1. The frequency f 0 − f orb corresponds to the beat signal.
Paper: Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
Authors: J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui
Figure caption: LT (left) and LOT (right) light curves folded with the orbital periods for the data taken in 2022 August and November, respectively. The orbital modulations are removed from the data. The solid lines show a sinusoidal function with a modulation frequency of f 0 = 147.40 days−1 for the LT data and f 0 = 149.35 days−1 for the LOT data. For the LOT data, the O − C curve of the phase of the pulsed peak is presented. The calculated amplitude (a) of the modulation for each data set is presented at the top of each panel.
Paper: Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
Authors: J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui
Figure caption: The O − C curves for the arrival phase of the 9.77 minutes periodic signal using the TESS data. The light curve is folded with the frequency of f 0 = 147.28 days−1 for the 2021 July/August data (left panel) and f 0 = 147.40 days−1 for the 2022 August data (right panel). A Gaussian function is applied to fit the pulse profile. In the right panel, the solid curve is the fitting of the O − C curve and indicates the first time derivative of the period of ﹩{\dot{P}}_{0}=1.2(5)\times {10}^{-7}﹩.
Paper: Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
Authors: J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui
Figure caption: LS periodograms for the 2021 July/August (right) and 2022 August TESS data after subtracting the orbital modulation and the data taken at the orbital phase of ϕ orb  =  0 − 0.2/0.8 − 1, where the periodic signal can be confirmed in the TESS data. The solid lines and dashed lines correspond to FAP = 0.1 and 0.01, respectively, as estimated by the methods of Baluev (2008).
Paper: Hours-long Near-UV/Optical Emission from Mildly Relativistic Outflows in Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Alexander Tchekhovskoy, Francois Foucart, Daniel Kasen, Rosalba Perna, Eliot Quataert, Brian D. Metzger
Figure caption: First row: bolometric luminosity in different models at  θ obs = 40° (left) and at various viewing angles in model T  s  (right). Second row: g-band magnitude (λ = 475 nm) of different models at  θ obs = 40° (left) and  θ obs = 90° (right). Thin dashed lines represent the contribution of r-process heating outside of the trapping radius. Third row: NUV (λ NUV = 250 nm), g (λ  g  = 475 nm), i (λ  i  = 760 nm), and K (λ  K  = 2160 nm) bands for model P  w  at  θ obs = 40° (left) and  θ obs = 90° (right). Fourth row: different angles in the g band for model T  s  (left) and P  w  (right). The light curves are shown in absolute magnitude (left y-axis) and apparent magnitude at 200 Mpc (right y-axis).
Paper: Hours-long Near-UV/Optical Emission from Mildly Relativistic Outflows in Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Alexander Tchekhovskoy, Francois Foucart, Daniel Kasen, Rosalba Perna, Eliot Quataert, Brian D. Metzger
Figure caption: The 3D renderings of the final snapshot of each simulation. The outflows in the poloidal field configurations reach r ≈ ct  f , and in model T  s , the outflow front is at r = 8.8 × 1010 cm. The blue parts display the asymptotic proper velocity, showing the sub- and mildly relativistic cocoon (dark) enveloping the relativistic jets (light). The red and yellow components portray the mass density, showing the merger ejecta and the accretion disk components, respectively. See full movies of models T  s  and P  c  at http://www.oregottlieb.com/bhns.html.
Paper: Hours-long Near-UV/Optical Emission from Mildly Relativistic Outflows in Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Alexander Tchekhovskoy, Francois Foucart, Daniel Kasen, Rosalba Perna, Eliot Quataert, Brian D. Metzger
Figure caption: Top: dimensionless velocity profile at various polar angles, measured at ϕ = 0. Solid (dotted) lines represent outflows (inflows). Homologous material (v ∝ r) is seen at r ≳ 109.5 cm at most angles θ ≳ 20°. Around the jet (blue), the radial velocity profile is stochastic. Bottom: ϕ-averaged  Y e as a function of the polar angle at different radii, calculated from a BH–NS postmerger simulation with the M1 scheme, measured 0.15 s after the merger.
Paper: Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf
Authors: Joanne L Pledger, Michael M Shara
Figure caption: Color–magnitude diagram plotting 80–200 Myr PARSEC stellar evolutionary isochrones along with our progenitor candidate at a metallicity of log(O/H) + 12 = 8.58. The V–I plotted is a lower limit using the 100% detection limit of our F555W images, and as such we expect the true value to be farther to the right in this plot. We also note that the star will explode at the end of the evolutionary track. The reddening vector to show the effect of extinction is plotted in the lower right corner
Paper: Shock Cooling and Possible Precursor Emission in the Early Light Curve of the Type II SN 2023ixf
Authors: Griffin Hosseinzadeh, Joseph Farah, Manisha Shrestha, David J. Sand, Yize Dong, 一泽 董, Peter J. Brown, K. Azalee Bostroem, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Iair Arcavi, Joshua Haislip, Daichi Hiramatsu, Emily Hoang, D. Andrew Howell, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Michael Lundquist, Curtis McCully, Nicolas E. Meza Retamal, Maryam Modjaz, Megan Newsome, Estefania Padilla Gonzalez, Jeniveve Pearson, Craig Pellegrino, Aravind P. Ravi, Daniel E. Reichart, Nathan Smith, Giacomo Terreran, József Vinkó
Figure caption: Left: photometry of SN 2023ixf from serendipitous imaging of the Pinwheel Galaxy in the days leading up to discovery by Itagaki (2023). Apart from the ATLAS (o) and ZTF (g) points, all the photometry in this panel is derived from unfiltered or color (Bayer RGB) images, and no offset is applied. For clarity, error bars are not plotted, and nondetections are marked with a downward-pointing arrow. The black curve shows an extrapolation of our earliest V-band data, assuming F  ν  ∝ t 2. This extrapolation is in severe disagreement with the data in this panel. Right: multiband photometry of SN 2023ixf from Las Cumbres Observatory, the Distance Less Than 40 Mpc (DLT40) Survey, and other sources reported to the Transient Name Server. The white diamonds show the data in the left panel and have no offset applied. The black curve again shows an extrapolation of our earliest V-band data, assuming F  ν  ∝ t 2. This extrapolation is a good description of the early V-band data but predicts a much later explosion time than is indicated by the pre-discovery observations.(The data used to create this figure are available.)
Paper: Shock Cooling and Possible Precursor Emission in the Early Light Curve of the Type II SN 2023ixf
Authors: Griffin Hosseinzadeh, Joseph Farah, Manisha Shrestha, David J. Sand, Yize Dong, 一泽 董, Peter J. Brown, K. Azalee Bostroem, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Iair Arcavi, Joshua Haislip, Daichi Hiramatsu, Emily Hoang, D. Andrew Howell, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Michael Lundquist, Curtis McCully, Nicolas E. Meza Retamal, Maryam Modjaz, Megan Newsome, Estefania Padilla Gonzalez, Jeniveve Pearson, Craig Pellegrino, Aravind P. Ravi, Daniel E. Reichart, Nathan Smith, Giacomo Terreran, József Vinkó
Figure caption: Fitting the shock-cooling model of Morag et al. (2023) to the multiband light curve of SN 2023ixf. Markers show the observed photometry, and solid lines are 100 model realizations randomly drawn from the posterior distribution. The vertical dotted line shows the best-fit t 0 from the shock-cooling model. The SN was detected for nearly a day before this time.
Paper: Shock Cooling and Possible Precursor Emission in the Early Light Curve of the Type II SN 2023ixf
Authors: Griffin Hosseinzadeh, Joseph Farah, Manisha Shrestha, David J. Sand, Yize Dong, 一泽 董, Peter J. Brown, K. Azalee Bostroem, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Iair Arcavi, Joshua Haislip, Daichi Hiramatsu, Emily Hoang, D. Andrew Howell, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Michael Lundquist, Curtis McCully, Nicolas E. Meza Retamal, Maryam Modjaz, Megan Newsome, Estefania Padilla Gonzalez, Jeniveve Pearson, Craig Pellegrino, Aravind P. Ravi, Daniel E. Reichart, Nathan Smith, Giacomo Terreran, József Vinkó
Figure caption: SN 2023ixf occurred in a spiral arm of the Pinwheel Galaxy near several star-forming regions. This image was made using 12 hr of small telescope data on the nights of 2023 May 20, 21, and 22. Image credit: Travis Deyoe, Mount Lemmon SkyCenter, University of Arizona.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: The spectrum of CEERS_1019 obtained with JWST/NIRCam’s wide-field slitless spectroscopy mode. This consists of spectra with both the column (“C”; blue) and row (“R”; purple) grisms, both taken with the F356W blocking filter, with a combined spectrum shown in black. While these data have a higher noise level than the NIRSpec spectra, we observe detections of the same [O II]3727+3729,  [Ne III]3870, and bluer Balmer lines that we see in NIRSpec (Figure 5). While we do not use the grism measurements in this paper, these data highlight the utility of this mode for obtaining slitless measurements of modestly faint emission lines out to high redshifts.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Comparison of the JWST/NIRSpec combined M grating spectrum when using the native pipeline pathloss correction (black) vs. without this step of the pipeline, but rather scaling the spectra to the measured JWST/NIRCam photometry (blue), as described in Fujimoto et al. (2023) and in Section 2.1.1. Our scaled spectrum (purple) highlights how the default pipeline pathloss correction underpredicts the total slit-loss correction for this source and that corrections to the NIRSpec spectrum are required for the flux calibration of resolved sources.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: 2D and 1D spectra of CEERS_1019 from three JWST/NIRSpec M gratings: G140M (top), G235M (middle), and G395M (bottom). The horizontal red dashed line identifies the central location of the source in the 2D spectrum and is the extraction center for our 1D spectra. Measured emission lines are indicated with purple dotted lines and discussed in Section 4. A description of the CEERS NIRSpec observations for this source is given in Section 2.1, and the data reduction process is described in Section 2.1.1.