Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization*

López-Rodríguez, Enrique; Clarke, Melanie; Shenoy, S.; Vacca, William D.; Coudé, Simon; Arneson, Ryan; Ashton, Peter; Eftekharzadeh, Sarah; Beck, Rainer; Beckman, J. E.; Borlaff, Alejandro S.; Clark, Susan; Dale, Daniel A.; Martin-Alvarez, Sergio; Ntormousi, Evangelia; Reach, W. T.; Román-Duval, Julia; Tassis, Konstantinos; Harper, D. A.; Marcum, Pamela M.

doi:10.3847/1538-4357/ac83ac

Cited by 19 publications

(21 citation statements)

References 31 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As a result, the light they emit in infrared wavelengths is polarized, with the polarization direction perpendicular to the mean direction of the magnetic field. Only recently has it been possible to trace extragalactic magnetic fields with this method (e.g.,the recent survey by Lopez-Rodriguez et al 2022).…”

Section: Observational Tracers Of Galactic Magnetic Fieldsmentioning

confidence: 99%

Galactic Dynamos

Brandenburg¹,

Ntormousi²

2022

Preprint

View full text Add to dashboard Cite

Spiral galaxies, including the Milky Way, have large-scale magnetic fields with significant energy densities. The dominant theory attributes these magnetic fields to a large-scale dynamo. We review the current status of dynamo theory and discuss various numerical simulations designed to explain either particular aspects of the problem or to reproduce galactic magnetic fields globally. Our main conclusions can be summarized as follows.

show abstract

Section: Observational Tracers Of Galactic Magnetic Fieldsmentioning

confidence: 99%

Galactic Dynamos

Brandenburg¹,

Ntormousi²

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…The observations were reduced using the same pipeline scheme as described in SALSA III (Lopez-Rodriguez et al 2022a). The final data products contain the Stokes IQU, polarization fraction (P), position angle of polarization (PA), polarized intensity (PI), and their uncertainties, with a pixel scale equal to the detector pixel scale, 6 9, at 154 μm.…”

Section: Far-infrared Polarimetric Observationsmentioning

confidence: 99%

“…The flux calibration uncertainty is estimated to be 8%. We also included the intrinsic polarization uncertainty of 0.2% and angular uncertainty of 3°of HAWC+ (Harper et al 2018;Lopez-Rodriguez et al 2022a). Note that our analysis is performed with polarization measurements having P/σ P 3, which ensures an uncertainty in the angle of polarization of 9°.6.…”

Section: Far-infrared Polarimetric Observationsmentioning

confidence: 99%

Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies*

López-Rodríguez

Borlaff

Beck

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

Mergers are thought to be a fundamental channel for galaxy growth, perturbing the gas dynamics and the magnetic fields (B-fields) in the interstellar medium (ISM). However, the mechanisms that amplify and dissipate B-fields during a merger remain unclear. We characterize the morphology of the ordered B-fields in the multiphase ISM of the closest merger of two spiral galaxies, the Antennae galaxies. We compare the inferred B-fields using 154 μm thermal dust and 11 cm radio synchrotron emission polarimetric observations. We find that the 154 μm B-fields are more ordered across the Antennae galaxies than the 11 cm B-fields. The turbulent-to-ordered 154 μm B-field increases at the galaxy cores and star-forming regions. The relic spiral arm has an ordered spiral 154 μm B-field, while the 11 cm B-field is radial. The 154 μm B-field may be dominated by turbulent dynamos with high 12CO(1–0) velocity dispersion driven by star-forming regions, while the 11 cm B-field is cospatial with high H i velocity dispersion driven by galaxy interaction. This result shows the dissociation between the warm gas mainly disturbed by the merger, and the dense gas still following the dynamics of the relic spiral arm. We find a ∼8.9 kpc scale ordered B-field connecting the two galaxies. The base of the tidal tail is cospatial with the H i and 12CO(1–0) emission and has compressed and/or sheared 154 μm and 11 cm B-fields driven by the merger. We suggest that amplified B-fields, with respect to the rest of the system and other spiral galaxies, may be supporting the gas flow between both galaxies and the tidal tail.

show abstract

“…The OTFMAP polarimetric mode has been successfully applied to galaxies such as Centaurus A (Lopez-Rodriguez 2021) and NGC 1097 (Lopez-Rodriguez et al 2021a), as well as the filamentary cloud L1495/B211 (Li et al 2021). The full description of the OTFMAP polarization mode of HAWC+ is described by Lopez-Rodriguez et al (2022a). Here we present a summary of the OTFMAP polarimetric observations and data reduction.…”

Section: Fir Polarimetric Observationsmentioning

confidence: 99%

On the Origin of Radio-loudness in Active Galactic Nuclei Using Far-infrared Polarimetric Observations

López-Rodríguez

Kishimoto

Antonucci

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

The dichotomy between radio-loud (RL) and radio-quiet (RQ) active galactic nuclei (AGNs) is thought to be intrinsically related to radio jet production. This difference may be explained by the presence of a strong magnetic field (B-field) that enhances, or is the cause of, the accretion activity and the jet power. Here we report the first evidence of an intrinsic difference in the polarized dust emission cores of four RL and five RQ obscured AGNs using 89 μm polarization with SOFIA/HAWC+. We find that the thermal polarized emission increases with the nuclear radio-loudness, R 20 = L 5GHz/L 20μm. The dust emission cores of RL AGNs are measured to be polarized, ∼5%–11%, while RQ AGNs are unpolarized, <1%. For RQ AGNs, our results are consistent with the observed region being filled with an unmagnetized or highly turbulent disk and/or expanding outflow at scales of 5–130 pc from the AGNs. For RL AGNs, the measured 89 μm polarization arises primarily from magnetically aligned dust grains associated with a 5–130 pc scale dusty obscuring structure with a toroidal B-field orientation highly offset, 65° ± 22°, with respect to the jet axis. Our results indicate that the size and strength of the B-fields surrounding the AGNs are intrinsically related to the strength of the jet power—the stronger the jet power is, the larger and stronger the toroidal B-field is. The detection of a ≤130 pc scale ordered toroidal B-field suggests that (a) the infalling gas that fuels RL AGNs is magnetized, (b) there is a magnetohydrodynamic wind that collimates the jet, and/or (c) the jet is able to magnetize its surroundings.

show abstract

Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization*

Cited by 19 publications

References 31 publications

Galactic Dynamos

Galactic Dynamos

Extragalactic Magnetism with SOFIA (SALSA Legacy Program): The Magnetic Fields in the Multiphase Interstellar Medium of the Antennae Galaxies*

On the Origin of Radio-loudness in Active Galactic Nuclei Using Far-infrared Polarimetric Observations

Contact Info

Product

Resources

About