Faraday rotation measure synthesis of UGC 10288 · Faraday rotation measure synthesis of UGC 10288...
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Faraday rotation measure synthesis of UGC 10288 Patrick Kamieneski 1 , Q. Daniel Wang 1 , Dylan Paré 1 , Kendall Sullivan 1 1 University of Massachusetts Amherst (on behalf of CHANG-ES collaboration) CHANG-ES INTRODUCTION Global configurations of magnetic fields in extragalactic sources are often explained by the prevailing -Ω dynamo mechanism. This involves the generation of large- scale regular field structures from small-scale turbulent fields in the ISM as they are subjected to differential rotation (as seen especially in spiral-type galaxies). These fields can be probed with radio polarization studies, and especially with rotation measures (or RMs), defined as the observed slope of the linear polarization angle vs. wavelength-squared, This effect, known as Faraday rotation, is introduced by the birefringence of magnetized plasma. RMs reveal both the magnitude and direction of line-of-sight fields in an intervening medium between the source and the observer, making them a remarkably useful metric. UGC 10288 • VLA observations from Continuum Halos in Nearby Galaxies– an EVLA Survey (CHANG-ES) • Edge-on galaxy UGC 10288 accompanied by a polarized complex background source (CHANG- ES A) perpendicular to foreground disk 1 (Fig. 1) • Faraday rotation of background source emission allows for probe of global magnetic field configuration in the disk and halo of UGC 10288 RESULTS • Less polarized emission detected at 20 cm, where one expects greater Faraday depolarization– the result of differential Faraday rotation within the bandwidth (see Fig. 2, 3) • Spatial distribution of RMs varies smoothly (existence of a large-scale mag. field) • Sign of RMs changes from negative, near the southernmost regions of CHANG-ES A (~ 1.0 kpc in projected distance from disk), to positive near core of double-lobed source (~2.5 kpc from disk) • Corresponds to a reversal in azimuthal magnetic field in halo (see Fig. 4, 5) IMPLICATIONS FOR -Ω D YNAMO THEORY • Analytic solutions to -Ω dynamo mechanism suggest existence of azimuthal modes and even/odd symmetry away from disk’s midplane • Symmetry of disk field tends to match that of halo, as one commandeers the other 3 • Fletcher+2011 also find evidence for a field reversal between disk and halo of M51 4 • Moss+2010 find using simulations that the mixed- parity solutions (even symmetry in disk, odd symmetry in halo, or vice versa) can only be explained via inclusion of a galactic wind 3 REFERENCES 1 Irwin J., et al., 2013, AJ, 146, 164 2 Brentjens M. A., de Bruyn A. G., 2005, A&A, 441, 1217 3 Moss D., et al., 2010, A&A, 512, A61 4 Fletcher A., et al., 2011, MNRAS, 412, 2396 [email protected] ROTATION MEASURE SYNTHESIS • Allows probe of more general quantity than RMs, known as Faraday depth, can relax the simplifying assumption of a single uniform Faraday-rotating medium 2 • Proportional to field strength, weighted by density, along the LOS: • Essentially a Fourier transform from 2 to φ-space • Outperforms “traditional” method (a least- squares fit) for sources with low SNR, large RMs 2 Fig. 1: Spitzer 3.6m image of UGC 10288 shown in grayscale, with JVLA C-array 6 cm linear polarization contours at 7.08 Jy/beam (1) x [3,6] Fig. 2, left: JVLA C-array 6 cm linear polarization image of CHANG-ES A. White vectors show B-field orientation, determined from polarization position angle (and uncorrected for Faraday rotation). Beam size is illustrated in white at lower left. Contours indicate approximate position of foreground disk. Fig. 3, right: As in Fig. 2, but JVLA B-array at 20 cm. Fig. 4, left: Rotation measure distribution from JVLA C-array 6 cm data, as determined via RM-synthesis. Fig. 5, right: As in Fig. 4, but using the simpler, “traditional” least-squares fitting method. Discrepancies are greatest in regions of weakest polarized intensity. Fig. 6, right: Sample least- squares fit determination of RM for a single LOS: RM ~ -153 ± 46 rad m -2 , reduced 2 = 0.29, d.o.f. = 14. Compare with result from RM-synthesis, RM ~ -128 ± 6.5 rad m -2 . SUMMARY • Faraday rotation of a source in the background of a nearby galaxy may help to reveal underlying magnetic fields in the foreground halo • In UGC 10288, we find a field reversal between edge-on disk and halo, an example of mixed- parity configuration caused by galactic winds 347.49 6 Jan. 2017
Transcript of Faraday rotation measure synthesis of UGC 10288 · Faraday rotation measure synthesis of UGC 10288...
FaradayrotationmeasuresynthesisofUGC10288PatrickKamieneski1,Q.DanielWang1,DylanParé1,KendallSullivan1
1UniversityofMassachusettsAmherst(onbehalfofCHANG-EScollaboration)
CHANG-ES
INTRODUCTIONGlobal configurations of magnetic fields in extragalactic sources are often explained by the prevailing 𝛼-Ω dynamo mechanism. This involves the generation of large-scale regular field structures from small-scale turbulent fields in the ISM as they are subjected to differential rotation (as seen especially in spiral-type galaxies). Thesefields can be probed with radio polarization studies, and especially with rotation measures (or RMs), defined as the observed slope of the linear polarization angle vs.wavelength-squared, This effect, known as Faraday rotation, is introduced by the birefringence of magnetized plasma. RMs reveal both themagnitude and direction of line-of-sight fields in an intervening medium between the source and the observer, making them a remarkably useful metric.
UGC10288• VLA observations from Continuum Halos in
Nearby Galaxies– an EVLA Survey (CHANG-ES)• Edge-on galaxy UGC 10288 accompanied by a
polarized complex background source (CHANG-ES A) perpendicular to foreground disk1 (Fig. 1)
• Faraday rotation of background source emissionallows for probe of global magnetic fieldconfiguration in the disk and halo of UGC 10288
RESULTS• Less polarized emission detected at 20 cm, where
one expects greater Faraday depolarization– theresult of differential Faraday rotation within thebandwidth (see Fig. 2, 3)
• Spatial distribution of RMs varies smoothly(existence of a large-scale mag. field)
• Sign of RMs changes from negative, near thesouthernmost regions of CHANG-ES A (~ 1.0 kpcin projected distance from disk), to positive nearcore of double-lobed source (~2.5 kpc from disk)
• Corresponds to a reversal in azimuthal magneticfield in halo (see Fig. 4, 5)
IMPLICATIONS FOR 𝛼-Ω DYNAMO THEORY• Analytic solutions to 𝛼-Ω dynamo mechanism
suggest existence of azimuthal modes andeven/odd symmetry away from disk’s midplane
• Symmetry of disk field tends to match that ofhalo, as one commandeers the other3
• Fletcher+2011 also find evidence for a fieldreversal between disk and halo of M514
• Moss+2010 find using simulations that the mixed-parity solutions (even symmetry in disk, oddsymmetry in halo, or vice versa) can only beexplained via inclusion of a galactic wind3
REFERENCES1 Irwin J., et al., 2013, AJ, 146, 1642 Brentjens M. A., de Bruyn A. G., 2005, A&A, 441, 12173Moss D., et al., 2010, A&A, 512, A614Fletcher A., et al., 2011, MNRAS, 412, 2396
ROTATION MEASURE SYNTHESIS• Allows probe of more general quantity than RMs,
known as Faraday depth, can relax thesimplifying assumption of a single uniformFaraday-rotating medium2
• Proportional to field strength, weighted bydensity, along the LOS:
• Essentially a Fourier transform from 𝜆2 to φ-space• Outperforms “traditional” method (a least-
squares fit) for sources with low SNR, large RMs2
Fig. 1: Spitzer 𝜆3.6𝜇m image of UGC 10288
shown in grayscale, with JVLA C-array 6 cm linear polarization contours at
7.08 𝜇Jy/beam (1𝜎) x [3,6]Fig. 2, left: JVLA C-array 6 cm linear polarization image of CHANG-ES A. Whitevectors show B-field orientation, determined from polarization position angle(and uncorrected for Faraday rotation). Beam size is illustrated in white at lowerleft. Contours indicate approximate position of foreground disk.Fig. 3, right: As in Fig. 2, but JVLA B-array at 20 cm.
Fig. 4, left: Rotation measure distribution from JVLA C-array 6 cm data, asdetermined via RM-synthesis.Fig. 5, right: As in Fig. 4, but using the simpler, “traditional” least-squares fittingmethod. Discrepancies are greatest in regions of weakest polarized intensity.
Fig. 6, right: Sample least-squares fit determinationof RM for a single LOS:RM ~ -153 ± 46 rad m-2,reduced 𝜒2 = 0.29, d.o.f. =14. Compare with resultfrom RM-synthesis, RM ~-128 ± 6.5 rad m-2.
SUMMARY• Faraday rotation of a source in the background
of a nearby galaxy may help to reveal underlyingmagnetic fields in the foreground halo
• In UGC 10288, we find a field reversal betweenedge-on disk and halo, an example of mixed-parity configuration caused by galactic winds
347.496Jan.2017
