adsabs/AstroCLIMB huggingface dataset:
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Left: the Simons Observatory Large Aperture Telescope Receiver Tester (LATR-Tester or LATRt) cryostat is shown in context with the Instrument Mounting Structure. The mounting structure has integrated XY stages that were used to move the different optical test equipment described throughout this paper. The structure was designed so it could be easily rolled over the LATRt cryostat after test equipment was installed, significantly simplifying the process of changing between types of measurements. Right: the LATR-Tester cross section with a single integrated optics tube and associated front-end filtering, indicated by the dashed box. Light enters through a high-density polyethylene window, travels through a series of double-sided infrared-blocking filters (DSIR), including one alumina IR-blocking filter, and passes through the 4 K low-pass-edge (LPE) mesh filter. The light is focused on the detector arrays by the three lenses, with two additional low-pass-edge filters near the 1 K and 100 mK stages. The optics tube components are further described in A. M. Kofman et al. (2024, in preparation) and N. Zhu et al. (2021).
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: The NDF can be mounted at either the 4 K or 100 mK optics tube stage. Left: the segmented NDF mounting plate shown in its initial mounting position (Cooldowns 1 and 2) at the 4 K end of the optics tube with two NDF filters installed. Right: a color coding of the pixels of one detector array indicating which pixels are expected to be unobstructed (green), partially obstructed (yellow), and fully obstructed (red) by the segmentation of the NDF mounting plate at its final mounting position (Cooldowns 3 and 4) of 20 mm from the focal plane at the sky side of the 100 mK low-pass edge filter.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Left: the Simons Observatory large aperture telescope is a 6 m crossed-Dragone telescope with a large field of view designed to illuminate over 60,000 detectors. Right: the large aperture telescope receiver (LATR) couples light from the sky via the telescope’s two primary mirrors. When fully populated, the receiver holds 13 optics tubes. Each optics tube is sensitive to one of three dichroic passbands: 30/40 GHz (low frequency), 90/150 GHz (mid-frequency), and 220/280 GHz (ultrahigh frequency). The goal of the LATR-Tester program is to fully test and validate each type of optics tube prior to deployment on the large aperture telescope. The optics tube location in the LATR is outlined by an orange dashed line, with details of the optics tube components shown in Figure 2.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Test equipment that was built and used for testing on the LATR-Tester includes (a) Fourier-transform spectrometer (FTS), (b) frequency-tunable laser source (FLS), (c) radio holography source, (d) thermal chopped source, (e) internal beam-filling cold load, and (f) external beam-filling warm load. Equipment (a)–(d) mount to XY stages on the surrounding instrument mounting structure, allowing them to be scanned across the optics tube’s field of view.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: The atmospheric emission expected at the Chilean site for an elevation of 50° modeled using the am code (S. Paine 2023). This emission is shown for increasing values of precipitable water vapor (PWV). In Table 2, we define the spectral regions that we use to evaluate out-of-band leakage, which are indicated in this figure by the highlighted and labeled regions.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Single pixel measurements used for NDF calibration, consisting of two 90 GHz and two 150 GHz detectors. Each curve shows the ratio of measurements taken with and without the NDF in front of the detectors. The NDF frequency dependence was fitted after combining all four detector ratio data sets. The gray band represents the uncertainty in the fit to the transmission function in Equation (1). Oscillations in the ratio curves are likely due to swapping from an alumina filter without an antireflection coating in Cooldown 1 to a filter with an antireflection coating in Cooldown 2.