adsabs/AstroCLIMB huggingface dataset:
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: CO Isotopologue line detection. The bottom-left panel illustrates the 12CO(1–0) moment-0 map in units of K km s−1. The other three panels present the line emission spectra for three selected pointings in the galaxy. The spectra are each plotted with an incrementing offset, from the top-left to the bottom-right panel, of ΔT mb = 5 K, 2 K, and 4 K, respectively. We scale the 13CO and C18O spectra by a factor of 5 or 10 such that the line emission is visible when compared to the much brighter 12CO line.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: CO isotopologue ratio trends. These panels show the line ratio as a function of galactocentric radius (left panel), SFR surface density (middle panel), and FWHM of 12CO(1–0) (right panel) panel. Only lines of sight within the NOEMA FOV are considered. We show the individual sight lines where both lines have S/N ≥ 5 as colored points. The small black triangles indicate 5σ upper limits. In addition, the orange line depicts the stacked line ratio trend. We stack all points for which 12CO(1–0) is significantly detected. The red line in the left panels is the radial trend obtained at low-angular resolution from (dB22). The red shaded region in the right panels indicates where the FWHM is below two times the channel width of our data (10 km s−1). The histograms show the distribution of these significantly detected data points per line ratio. The black line represents the weighted average (weighted by the 12CO(1–0) intensity), and the dotted lines represent the weighted 16th-to-84th percentile range.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Correlations of the LTE-based parameters. (Left panel) We compute the 13CO column density, ﹩{N}_{\mathrm{LTE}}\left({}^{13}\mathrm{CO}\right)﹩ based on the 13CO(1–0) integrated intensity using Equation (4), which assumes LTE. Only sight lines were used where the 13CO(1–0) line emission is significantly detected (S/N ≥ 5). (Right panel) The CO-to-H2 conversion factor for the 12CO(1–0) emission as a function of galactocentric radius assuming [13CO/H2]=1.7 × 10−6. The red circles show binned values. The shaded red area represents the ±1σ scatter per bin. For reference, we also present the local neighborhood value of 4.3 (black line) and the average value derived from our non-LTE analysis (red line). In the bottom-right corner of each panel, we present the average error for a single data point, based on the MC resampling approach. In the left panel, points are color-coded based on their density in the panel (this is a qualitative representation of how densely the points are distributed in the parameter space).
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Distribution of LTE-derived parameter values. (Top row panels) The maps illustrate the distribution of the excitation temperature, T ex (left panel), the beam filling factor, ϕ (center panel), and the 13CO optical depth (right panel), across the inner region of M51. The contours indicate the 12CO(1–0) integrated intensities ranging from 40–200 K km s−1 in steps of 40 K km s−1. (Bottom row panels) The panels present the distribution of the excitation temperature (T ex), the beam filling factor (ϕ), the optical depth of 13CO (τ 13), and the 13CO column density (N LTE(13CO)). The median and 16th-to-84th percentile range are indicated in the upper corner of each panel. The beam filling factor is set to 1 if the derived value exceeds unity. This causes a pile-up (indicated in orange) in the distribution. Optical depth values below log10(τ) < −1 (left of the red vertical line) can be considered as optically thin.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: CO isotopologue ratio trends (continued). These panels have the same description as in Figure 3.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Spatial distribution of the maximum likelihood model. These panels show the pixel-wise maximum likelihood value derived from the χ 2 minimization approach. (Left panel) The kinetic temperature, T kin, map. The contours show the integrated 12CO(1–0) intensity isophote at 20, 50, 100, and 200 K km s−1. The blue-dashed circle indicates 20″ in radius, which we use to differentiate between center and disk. (Second-from-left panel) The distribution of the mean volume density, ﹩{n}_{{{\rm{H}}}_{2}}﹩, from which the CO emission is originating. (Middle panel) The 12CO column density map. (Second-from-the-right panel) The beam filling factor. (Right panel) The abundance ratio of 12CO-to-13CO map. We note that we only have solutions for pixels where all four lines (12CO and 13CO (1–0), (2–1)) are significantly (>5σ) detected.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Radial trend of the non-LTE-derived CO-to-H2 conversion factor. We find overall a flat trend of ﹩{\alpha }_{{}^{12}\mathrm{CO}(1-0)}﹩ with galactocentric radius. The orange points show the value for the individual sight lines. The purple points depict the radially binned average. We illustrate the scatter of the radially binned values using the purple shade. The galaxy-wide average based on a dust-based technique by J. S. den Brok et al. (2023b) is represented by the blue horizontal line. The red horizontal line represents our LTE-derived average α CO.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Optical depth of 12CO and the ﹩{R}_{10}^{13/12}﹩ line ratio. The points are color-coded with respect to the sight line’s corresponding integrated 12CO(1–0) line brightness. We perform a linear regression (in log-log space; blue line), which highlights the positive relation (Pearson’s correlation coefficients indicated in top-left corner) with the ﹩{R}_{10}^{13/12}﹩ line ratio.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: Comparing LTE and non-LTE-derived parameters. (Left panel) Contrasting the optical depth of 13CO(1–0). The points are color-coded by their parameter-space filling based on a 2D Gaussian kernel function. The black dashed line illustrates the 1:1 relation. (Right panel) Comparing the total 13CO column density derived using the LTE and non-LTE approach. The panel description follows the left one.
Paper: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H2 Conversion Factors in M51
Authors: Jakob den Brok, María J. Jiménez-Donaire, Adam Leroy, Eva Schinnerer, Frank Bigiel, Jérôme Pety, Glen Petitpas, Antonio Usero, Yu-Hsuan Teng, Pedro Humire, Eric W. Koch, Erik Rosolowsky, Karin Sandstrom, Daizhong Liu, Qizhou Zhang, Sophia Stuber, Mélanie Chevance, Daniel A. Dale, Cosima Eibensteiner, Ina Galić, Simon C. O. Glover, Hsi-An Pan, Miguel Querejeta, Rowan J. Smith, Thomas G. Williams, David J. Wilner, Valencia Zhang
Figure caption: The 1D and 2D marginalized likelihood distributions. The red (left panel) and blue (right panel) corner plots show the resulting 1D and 2D likelihood probability density function (PDF) from χ 2 minimization following Equation (7). The map in the center illustrates the 13CO(2–1) integrated intensity with the sight lines highlighted for which the two corner plots are calculated.
Paper: Searching for Planets Orbiting Vega with the James Webb Space Telescope
Authors: Charles Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Marie Ygouf, Alexandra Greenbaum, Jarron Leisenring, Andras Gaspar, John Krist, George Rieke, Schuyler Wolff, Kate Su, Klaus Hodapp, Michael Meyer, Doug Kelly, Martha Boyer, Doug Johnstone, Scott Horner, Marcia Rieke
Figure caption: (Top) the full-frame F444W image generated using ADI. The dark holes bracketing each bright source are an expected artifact of the roll subtraction and serve as a check for the reality of each object. The eight brightest F444W sources within 60″ of Vega and not obviously extended are indicated (Table 4). In the figure north is up and east is to the left. The large circles delineate features seen in the MIRI data (K. Y. L. Su et al. 2024, in preparation): the dotted yellow circle denotes the outer extent of the halo seen in the F2550W image (33″), the blue circles denote the extent of the Kuiper Belt analog seen in both MIRI and ALMA (10″–22″), an inner disk extends inward to the star, while the dotted green ring marks the location of a dip in the dust distribution seen around 5″–10″. Small yellow circles denote Gaia sources brighter than G < 18 mag. (Bottom) full-frame image for F210M, with PSF subtraction performed with ADI + RDI. The many dark spots represent sources in the field of the reference image. Intensity units are in MJy sr−1.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Allan deviance of the two transit and two eclipse white-light curves. Note that the F322W2 eclipse, the only visit that uses two groups, has substantially higher rms than all other visits at high bin sizes. However, this visit uses a read pattern of BRIGHT2, so the two groups consist of two averaged reads each; whereas the F322W2 transit uses three groups with the BRIGHT1 pattern, for a total of only three reads.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Best-fit transmission (left) and emission (right) spectra of HD 189733b, from four NIRCam transit observations. The black line indicates the best-fit model from PLATON retrievals, while the colored lines indicate the effect of removing a single opacity source (e.g., the opacity of a single molecule) from the best-fit model.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Posterior distributions inferred from full equilibrium chemistry retrievals. Left: metallicity and C/O ratio inferred from the NIRCam transmission spectrum (purple), the NIRCam emission spectrum (brown), and the combined pre-JWST transmission and emission spectra (black). Right: posterior distributions inferred from the F322W2 transmission spectrum (blue), F444W transmission spectrum (orange), F322W2 emission spectrum (green), and F444 emission spectrum (red). In both subplots, 1σ and 2σ contours are plotted. Note that the F444W transit posterior has a second mode at very high metallicity (∼200×), which is outside the range of this plot.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Same as Figure 5, except that a methane multiple is now a free parameter in all retrievals in order to account for possible methane depletion. For the joint pre-JWST transit and eclipse retrieval (left, black), we only applied the methane multiple to the transmission spectrum. Just as for Figure 5, the F444W transit posterior has a second mode at very high metallicity (∼200×), which is outside the range of this plot.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Binned white-light curve of the eclipse observation in the F322W2 filter (left) and the F444W filter (right), with the best-fit systematics model divided out, the best-fit eclipse model plotted on top, and the residuals at the bottom. Note the significantly worse correlated noise in the bluer band.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Comparison of the eclipse depths in the overlap region between the two filters. The curves indicate the system throughput for the two filters. Note the large discrepancy for the reddest bin, and the sharp drop-off of the F322W2 throughput at that wavelength.
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Comparison of the fiducial transmission spectrum adopted by G. Fu et al. (2024) to that adopted by the present paper (dark colors).
Paper: Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era
Authors: Michael Zhang, Kimberly Paragas, Jacob L. Bean, Joseph Yeung, Yayaati Chachan, Thomas P. Greene, Jonathan Lunine, Drake Deming
Figure caption: Abundances of selected molecules as predicted by VULCAN, with photochemistry (dashed lines) and without (solid lines).
Paper: frb-voe: A Real-time Virtual Observatory Event Alert Service for Fast Radio Bursts
Authors: Thomas C. Abbott, Andrew V. Zwaniga, Charanjot Brar, Victoria M. Kaspi, Emily Petroff, Mohit Bhardwaj, P. J. Boyle, Amanda M. Cook, Ronniy C. Joseph, Kiyoshi W. Masui, Ayush Pandhi, Ziggy Pleunis, Paul Scholz, Kaitlyn Shin, Shriharsh Tendulkar
Figure caption: The three interactable backends (tns, voe, and subscriber) available to the operator of frb-voe. The backends can be accessed using a built-in CLI. As an example, publishing a VOEvent 1 is done by an HTTP request with URL set to  https://localhost:port/frb-voe/voe/create_voe .
Paper: frb-voe: A Real-time Virtual Observatory Event Alert Service for Fast Radio Bursts
Authors: Thomas C. Abbott, Andrew V. Zwaniga, Charanjot Brar, Victoria M. Kaspi, Emily Petroff, Mohit Bhardwaj, P. J. Boyle, Amanda M. Cook, Ronniy C. Joseph, Kiyoshi W. Masui, Ayush Pandhi, Ziggy Pleunis, Paul Scholz, Kaitlyn Shin, Shriharsh Tendulkar
Figure caption: A Histogram of the latencies of VOEvents broadcast between the start of the service’s operation (2021/10/08) and 2024/06/15. Detection VOEvents are shown in blue, and subsequent VOEvents are shown in red. The mean latency for each VOEvent type is shown in a dashed line and is between 12 and 13 s for both types. The slightly larger latency in subsequent type events may be due to an additional known source check in the real-time pipeline.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: TANDEM telescopes’ image quality diagnostics, according to Zemax OpticStudio modeling. The upper sequence displays a multiwavelength spot diagram at increasing radial distance (in degrees) from the optical axis, as labeled above each spot. Johnson–Cousins filters are color coded in the spots as B = blue, V = green, Rc = red, and Ic = violet. The pixel size is reported at the top left, as a reference. The lower plot displays the rms spot radius (in units of μm) along the radial distance from the CMOS center for a set of sampled wavelengths in the 4000–9000 Å range, as schematically color coded by the curves in the plot. The black curve refers to the polychromatic response, while the horizontal line at 1.91 μm is the diffraction limit set by the Airy disk. The 9 μm pixel size of the GSense 4040 CMOS is marked as a dashed red line, as labeled. The nominal figures do not take into account seeing broadening and mechanical tolerance in the optical system assembly.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: A diagnostic diagram for the optical design of the TANDEM telescopes. The 16% obstruction of the entrance pupil for the adopted size of the secondary mirror, placed at a distance (F − X) = 657 mm from the primary mirror, is marked by the blue dot. It is compared with the expected obstruction for the size of the secondary mirror such as to intercept the paraxial optical beam only (blue curve) or the full FOV with no vignetting (brown curve). The nominal ratio W/L1 for the Wynne corrector train is also displayed, according to Equation (10) (the red curve refers to the right scale on the plot), compared with the adopted figure for the telescopes (red diamond). The red curve has to be regarded as an upper limit to the optimal optical combinations. See text for a full discussion of these quantities.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: Some of the predefined pointing patterns for the four TANDEM telescopes (each marked with a different color). As a reference, the celestial region around the Andromeda galaxy, M31, has been displayed, together with a full Moon sketch. Note in particular, in the lower panel, two very extended “sparse-field” options, one along a diagonal direction spanning a 12° × 2° FOV and the other consisting of four independent pointings each 20° apart.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: An illustrative sketch of the relevant parameters for TANDEM's optical design optimization. See text for a full discussion.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: The covered FOV of TANDEM in “collimated” configuration, with the four telescopes pointing at the same 2° × 2° field. The celestial region around the Andromeda galaxy, M31, is displayed as an illustrative reference, together with a full Moon sketch. Though with a smaller FOV, this configuration allows the observer to maximize TANDEM sensitivity, reaching a 0.75 mag deeper limit compared to imaging with a single telescope.
Paper: The TANDEM Project as a Pilot Case for Wide-field Telescope Arrays
Authors: A. Buzzoni, A. Carbognani, R. Di Luca, E. Diolaiti, R. Gualandi, A. Semola, G. M. Stirpe, F. Bonoli, I. Bruni, F. Cortecchia, I. Foppiani, S. Galleti, M. Lombini, L. Schreiber
Figure caption: Left panel: the adopted optical design for the Wynne corrector on board the TANDEM telescopes. The optical train is placed just in front of the CMOS detector (and the filter wheel), and intercepts the incoming optical beam from the secondary mirror of the Newtonian system, as sketched in the right panel.