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arxiv: 2605.23532 · v1 · pith:55FAQTK3new · submitted 2026-05-22 · 🌌 astro-ph.IM

Design and Development of Cassegrain Module for PARAS-2 Spectrograph (CAMPAS)

Kevikumar A. Lad , Neelam J. S.S.V. Prasad , Kapil Bharadwaj , Nikitha Jithendran , Ashirbad Nayak , Rishikesh Sharma , Abhijit G. Chakraborty , Vishal Joshi This is my paper

Pith reviewed 2026-05-25 02:46 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords Cassegrain modulefiber-fed spectrographatmospheric dispersion correctorfiber injectioninstrument designPARAS-2PRL 2.5m telescopecalibration unit
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The pith

CAMPAS module was designed and installed to couple the PRL 2.5 m telescope to the PARAS-2 spectrograph via focal reduction, fiber injection, and atmospheric dispersion correction.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reports the in-house design, construction, and 2022 installation of the Cassegrain Module for PARAS-2 (CAMPAS) at one of the side ports of the PRL 2.5 m telescope. CAMPAS functions as the optical interface that reduces the telescope focal ratio, corrects atmospheric dispersion, injects light into the spectrograph fibers, supplies calibration sources, and supports point-spread-function monitoring. The module comprises a focal reducer, beam-guiding optics, an atmospheric dispersion corrector, fiber mounts, and a calibration unit; all subsystems were developed between 2020 and 2022 to meet the stability and beam-quality requirements of the high-resolution echelle spectrograph.

Core claim

The central claim is that a custom Cassegrain module consisting of a focal reducer, atmospheric dispersion corrector, fiber mounts, calibration unit, and auxiliary optics has been successfully designed, fabricated, and installed to deliver precise, stable light injection from the PRL 2.5 m telescope into the fibers of the PARAS-2 spectrograph while also enabling PSF estimation and atmospheric dispersion correction.

What carries the argument

The CAMPAS Cassegrain module, whose focal reducer, atmospheric dispersion corrector, and fiber-injection optics together form the interface that matches the telescope output beam to the spectrograph input.

If this is right

  • The spectrograph can receive light with corrected atmospheric dispersion across its operating wavelength range.
  • Calibration lamps can be injected into the same optical path used for science observations.
  • Point-spread-function monitoring becomes available at the fiber entrance to track telescope and instrument performance.
  • The module supports the first-light operation of the PARAS-2 spectrograph on the PRL 2.5 m telescope.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar modular Cassegrain interfaces could be replicated for other fiber-fed spectrographs on mid-sized telescopes where atmospheric dispersion and fiber coupling stability are limiting factors.
  • The in-house development timeline of roughly two years indicates that comparable institutions could produce functional ADC-plus-fiber-feed units without external vendors.
  • Once operational, the module may enable science programs that require simultaneous calibration and dispersion-corrected spectra over long exposures.

Load-bearing premise

The selected optical layout and components will maintain the beam quality, stability, and throughput needed by the PARAS-2 spectrograph once mounted on the telescope.

What would settle it

On-sky measurements after installation that show the delivered fiber injection efficiency, residual atmospheric dispersion, or PSF stability falling short of the values required by the PARAS-2 spectrograph design.

Figures

Figures reproduced from arXiv: 2605.23532 by Abhijit G. Chakraborty, Ashirbad Nayak, Kapil Bharadwaj, Kevikumar A. Lad, Neelam J. S.S.V. Prasad, Nikitha Jithendran, Rishikesh Sharma, Vishal Joshi.

Figure 1
Figure 1. Figure 1: Schematic of the CAMPAS (not to scale) showing how starlight and a calibration light are [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Flowchart showing different activities related to the development of the CAMPAS. [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Opto-mechanical design of the CAMPAS: CAD model (Isometric View). [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Opto-mechanical design of the CAMPAS: CAD model - Top View showing different [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Optical layout of the star fiber feed system in the CAMPAS: The light from the telescope [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Geometric spot diagram at the star fiber tip across different field angles at 30 degrees [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: (a) Displacement at fiber tip as a function of telescope altitude at different rotator positions [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Schematic block diagram of the CAMPAS control system illustrating how the various [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: Schematic of the setup for the CAMPAS alignment. [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
Figure 9
Figure 9. Figure 9: Screenshot of GUI developed for the CAMPAS. [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: CAMPAS (marked with red box) installed on the PRL 2.5m Telescope. [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
read the original abstract

We present here the design and development of the CAMPAS, the Cassegrain Module for the PARAS-2 spectrograph. PARAS-2 is a high-resolution fiber-fed echelle spectrograph developed for the PRL 2.5m Telescope. The CAMPAS acts as a coupler between two optical systems, the PRL 2.5m telescope and the PARAS-2 spectrograph. It has primarily been developed for the precise injection of the light beam into the optical fibers of the PARAS-2 spectrograph. The CAMPAS consists of a focal reducer, beam-guiding optics, an atmospheric dispersion corrector, optical fiber mounts; a calibration unit incorporating calibration lamps and beam-guiding optics; and other auxiliary subsystems. It was developed in-house at PRL, Ahmedabad, between the years 2020-2022 and was installed at one of the two side ports of the PRL 2.5m telescope in March 2022. It is one of the first light instruments for the PRL 2.5m Telescope. The CAMPAS serves critical purposes of precise fiber feed, PSF estimation, and atmospheric dispersion correction.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript describes the design, development, and installation of the CAMPAS (Cassegrain Module for PARAS-2 Spectrograph), a coupler between the PRL 2.5m telescope and the PARAS-2 high-resolution fiber-fed echelle spectrograph. It details subsystems including a focal reducer, beam-guiding optics, atmospheric dispersion corrector (ADC), optical fiber mounts, a calibration unit with lamps, and auxiliary components. The module was built in-house at PRL from 2020-2022 and installed at a side port of the telescope in March 2022 as one of the first-light instruments, with the stated purpose of enabling precise fiber feed, PSF estimation, and atmospheric dispersion correction.

Significance. If the optical layout delivers the required beam quality and stability, CAMPAS would provide essential capabilities for high-resolution spectroscopy on the PRL 2.5m telescope, supporting precise light injection into fibers and correction for atmospheric effects. The in-house development from 2020-2022 represents a concrete engineering achievement for the project team.

major comments (1)
  1. [Abstract] Abstract: The central claim that CAMPAS 'serves critical purposes of precise fiber feed, PSF estimation, and atmospheric dispersion correction' is unsupported by any measured performance data. The manuscript provides only a descriptive account of the focal reducer, ADC, and fiber mounts with no reported values for coupling efficiency, PSF metrics, ADC residuals, beam stability, or on-sky verification results to confirm the layout meets PARAS-2 requirements.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the detailed review and constructive comment. The manuscript is a design and development paper focused on the in-house construction and installation of CAMPAS; we agree that the abstract's phrasing implies demonstrated performance that is not supported by data in the current text. We will revise the abstract to accurately reflect the design intent rather than achieved results.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that CAMPAS 'serves critical purposes of precise fiber feed, PSF estimation, and atmospheric dispersion correction' is unsupported by any measured performance data. The manuscript provides only a descriptive account of the focal reducer, ADC, and fiber mounts with no reported values for coupling efficiency, PSF metrics, ADC residuals, beam stability, or on-sky verification results to confirm the layout meets PARAS-2 requirements.

    Authors: We agree with the referee that the final sentence of the abstract overstates the module's demonstrated capabilities. The paper describes the optical design, mechanical implementation, and installation but does not contain on-sky verification or quantitative performance metrics. We will revise the abstract to state that CAMPAS is designed to enable precise fiber feed, PSF estimation, and atmospheric dispersion correction, removing any implication of measured performance. The revised sentence will read: 'The CAMPAS is designed to enable precise fiber feed, PSF estimation, and atmospheric dispersion correction.' No performance data will be added, as this manuscript is limited to the design and development phase. revision: yes

Circularity Check

0 steps flagged

No circularity: purely descriptive engineering report

full rationale

The manuscript is a design-and-development description of hardware components (focal reducer, ADC, fiber mounts, calibration unit) and their installation timeline. No equations, fitted parameters, performance predictions, or derivation chains appear in the provided text or abstract. The central claims are statements of purpose and construction history rather than quantitative results derived from inputs. No self-citations, ansatzes, or uniqueness theorems are invoked as load-bearing steps. The paper is therefore self-contained against external benchmarks with zero circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No mathematical model, free parameters, or invented physical entities are present; the work is purely descriptive engineering.

pith-pipeline@v0.9.0 · 5781 in / 938 out tokens · 17558 ms · 2026-05-25T02:46:55.864207+00:00 · methodology

discussion (0)

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