Planck an Overview of the Spacecraft

Abstract

The two science missions Herschel, an observatory-type mission, and Planck, a survey mission, are combined in one program within ESA's long-term science program. This paper deals with Planck. The objective for Planck is to image systematically the whole sky simultaneously with two scientific instruments in nine frequency channels between 30 and 900 GHz to unravel the temperature fluctuations, i.e. the anisotropy, of the cosmic background radiation. Both satellites, have been launched together from the European Space Port in Kourou, French Guiana, on a single Ariane 5 launcher, the orbits will be Lissajous orbits around the 2nd Lagrange Point, "so called" L2 of the Earth-Sun system.This paper gives an overview of the Planck spacecraft including the scientific instruments and the on ground testing.

Integrating Cosmic Microwave Background Readings with Celestial Navigation to Enhance Deep Space Navigation

“…For missions like Planck, approximately 35% of the satellite’s total power consumption and 32% of its total mass are attributed to the instruments [ 70 ]. Planck, for instance, had a total mass of 2000 kg and a power load of 1600 W [ 71 ]. This means the payload mass was estimated to be approximately 640 kg, and the power consumption was approximately 560 W.…”

Analysis of Orbital Configurations for Millimetron Space Observatory

“…As for the orbital configurations in the vicinity of the Lagrange point L2 of the Sun-Earth system, Millimetron will be the first mission with VLBI mode to conduct observations there. The following missions can be noted as example of successfully operated and operating space observatories at L2 point: WMAP, Planck, Herschel, GAIA, recently launched Spektr-RG [36] and the upcoming James Webb Space Telescope, WFIRST and others [37,38,39,40,41,42].…”

Observations of compact sources in galaxy clusters using MUSTANG2

“…Because of the unique spectral shape of the tSZE, it is possible to separate out the tSZE signal using multifrequency observations -in the case of ACT DR5, 90 and 150 GHz are used to find clusters. Other ground based experiments use similar bands while, due to the lack of atmospheric absorption, space based experiments such as Planck (Passvogel et al 2010) can have wider and more complete frequency coverage. Sets of matched filters (matched to 𝑔(𝑥) and the cluster profile) are used to extract maps of peak Compton-𝑦 with different filter sets being used to obtain maximum signal-to-noise (SNR) on clusters in different mass and redshift ranges (Hilton et al 2021).…”

“…One of the advantages of the tSZE is that its surface brightness is redshift independent, meaning that, given sufficient resolution, it is relatively easy to detect and study clusters at high redshifts where optical and X-ray methods need long exposure times. Experiments such as Planck (Passvogel et al 2010) and the South Pole Telescope (SPT) Benson et al (2014) have carried out deep surveys finding hundreds of clusters (Planck Collaboration et al 2014;Bleem et al 2020) and the recent data release from the Atacama Cosmology Telescope (ACT; Thornton et al 2016) contains 4195 optically confirmed clusters (Hilton et al 2021). In the future, experiments such as the Simons Observatory, CMB-S4, and CMB-HD expect to find an order of magnitude more clusters (Ade et al 2019;Abazajian et al 2016;Abazajian et al 2019;Sehgal et al 2019).…”