IRAS 04368+2557 — LLMpedia

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IRAS 04368+2557 is a young stellar object embedded in the Taurus Molecular Cloud near the dark nebula L1527, associated with a protostellar envelope and an edge-on circumstellar disk; it is often studied alongside other protostars such as HL Tauri, T Tauri, and L1551 IRS 5. The source has been observed across the electromagnetic spectrum by facilities including the Infrared Astronomical Satellite, the Submillimeter Array, and the Atacama Large Millimeter/submillimeter Array, and figures in comparative studies with objects like IRAS 16293-2422, VLA 1623-2417, and DG Tauri. As an embedded Class 0/I protostar in Taurus, it informs models of early stellar evolution developed by groups at institutions such as the Harvard–Smithsonian Center for Astrophysics, the Max Planck Institute for Astronomy, and the National Radio Astronomy Observatory.

Introduction

IRAS 04368+2557 is cataloged from the Infrared Astronomical Satellite all-sky survey and is located in the Taurus Molecular Cloud, a nearby star-forming region that includes notable sites like Barnard 18, L1536, and Heiles Cloud 2. The source is often referenced in observational programs conducted with the Spitzer Space Telescope, the Hubble Space Telescope, and ground arrays led by teams from the California Institute of Technology, the Smithsonian Astrophysical Observatory, and the European Southern Observatory. Studies frequently compare its properties to protostars such as HH 30, IRAS 04302+2247, and TMC-1A to constrain models proposed by researchers at the Kavli Institute for Theoretical Physics and the Institute for Astronomy, University of Hawaii.

Discovered in the 1980s by the Infrared Astronomical Satellite survey, IRAS 04368+2557 was subsequently targeted in follow-up campaigns with instruments on the IRTF, the James Clerk Maxwell Telescope, and the Very Large Array. Early infrared detections were placed in context with millimeter observations from the Owens Valley Radio Observatory and bolometer surveys by teams from the Max Planck Society; later high-resolution imaging by the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array resolved disk and envelope structures similar to those reported for HL Tauri and L1527 IRS. Spectroscopic programs at the Keck Observatory and the Very Large Telescope provided complementary data used by authors affiliated with the University of California, Berkeley and the University of Arizona.

Classified as a Class 0/I protostar in the scheme developed from work at the Jet Propulsion Laboratory and summarized in reviews from the Annual Review of Astronomy and Astrophysics, the object exhibits a bolometric temperature and spectral energy distribution consistent with very young accreting sources like IRAS 16293-2422 and VLA 1623. Estimates of its luminosity and envelope mass derive from radiative transfer models employed by research groups at the Max Planck Institute for Radio Astronomy and the CEA Saclay, and are compared with protostellar evolutionary tracks from the Geneva Observatory and the Padova group. Observational classification has been refined using criteria adopted at conferences organized by the International Astronomical Union and the American Astronomical Society.

High-resolution interferometric imaging reveals an edge-on disk and flattened envelope structure studied in analogy with disks around HL Tauri, HH 30, and IRAS 04302+2247; these analyses utilize radiative transfer codes from groups at the Max Planck Institute for Astronomy and the University of Cambridge. Millimeter continuum and molecular line maps from the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array show dust concentrations and infall signatures similar to those discussed in papers from the Harvard–Smithsonian Center for Astrophysics and the Institut d'Astrophysique de Paris. Polarimetric imaging with instruments on the Gemini Observatory and the Hubble Space Telescope constrains grain growth and envelope geometry in ways comparable to studies of B335 and L1527 IRS.

IRAS 04368+2557 drives molecular outflows and shows reflection nebulosity that are compared to protostellar jets seen in HH 212, HH 30, and L1551 IRS 5; CO and SiO line emission observed with the Submillimeter Array and the Plateau de Bure Interferometer trace these flows. Observations by groups at the National Radio Astronomy Observatory and the Max Planck Institute for Radio Astronomy show kinematic signatures analogous to those analyzed in surveys led by the Carnegie Institution for Science and the Leiden Observatory. The morphology of the associated nebula has been imaged by the Hubble Space Telescope and ground-based adaptive optics teams from the W. M. Keck Observatory and the European Southern Observatory.

Photometric monitoring with the Spitzer Space Telescope, the United Kingdom Infrared Telescope, and optical/infrared facilities operated by the Las Cumbres Observatory reveals variability linked to accretion bursts and extinction changes, similar to behaviors documented for FU Orionis objects and EXor-type variables studied at the Harvard–Smithsonian Center for Astrophysics and the Max Planck Institute for Astronomy. Time-series analyses published by collaborations including the Sloan Digital Sky Survey team and members of the AAVSO provide constraints on episodic accretion models advanced by theorists at the Princeton University and the University of Cambridge.

As a prototypical embedded source in Taurus, IRAS 04368+2557 is central to surveys of protostellar evolution conducted by consortia involving the Spitzer Science Center, the European Space Agency, and the National Science Foundation. Comparative work places it alongside benchmark objects like HL Tauri, TMC-1, and L1527 in efforts led by the Infrared Processing and Analysis Center and teams at the University of Leeds to map star formation efficiency, envelope dissipation, and disk formation. Its inclusion in multiwavelength campaigns coordinated with the James Webb Space Telescope planning groups and the Atacama Large Millimeter/submillimeter Array Large Programs continues to inform theoretical frameworks developed at the Institute for Advanced Study and the Kavli Institute.

Category:Protostars Category:Taurus Molecular Cloud Category:Young stellar objects