MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSRπ. I. TWO BINARY MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS

Deller, Adam T.; Vigeland, Sarah J.; Kaplan, David L.; Goss, W. M.; Brisken, Walter; Chatterjee, Shami; Cordes, J. M.; Janssen, G. H.; Lazio, T. Joseph W.; Petrov, Leonid; Stappers, B. W.; Lyne, A. G.

doi:10.3847/0004-637x/828/1/8

Cited by 38 publications

(50 citation statements)

References 48 publications

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“…2 o away is at the stateof-the-art, only comparable with 'in-beam' phase referencing observations with a calibrator ca. 10s of arcminutes away (Deller et al 2013(Deller et al , 2016. This improvement is expected to continue to apply at all angular scales.…”

Section: Discussionmentioning

confidence: 82%

MultiView High Precision VLBI Astrometry at Low Frequencies

Rioja

Dodson

Orosz

et al. 2017

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The arrival of the Square Kilometer Array (SKA) will revitalise all aspects of Very Long Baseline Interferometry (VLBI) astronomy at the lower frequencies. In the last decade there have been huge strides towards routinely achieving high precision VLBI astrometry at frequencies dominated by the tropospheric contributions, most notably at 22GHz, using advanced phase referencing techniques. Nevertheless to increase the capability for high precision astrometric measurements at low radio frequencies (<8 GHz) an effective calibration strategy of the systematic ionospheric propagation effects that is widely applicable is required. Observations at low frequencies are dominated by distinct direction dependent ionospheric propagation errors, which place a very tight limit on the angular separation of a suitable phase referencing calibrator.The MultiView technique holds the key to the compensation of atmospheric spatial-structure errors, by using observations of multiple calibrators and 2-D interpolation. In this paper we present the first demonstration of the power of MultiView using three calibrators, several degrees from the target, along with a comparative study of the astrometric accuracy between MultiView and phasereferencing techniques. arXiv:1612.02554v1 [astro-ph.IM] 8 Dec 2016-2 -MultiView calibration provides an order of magnitude improvement in astrometry with respect to conventional phase referencing, achieving ∼ 100micro-arcseconds astrometry errors in a single epoch of observations, effectively reaching the thermal noise limit.MultiView will achieve its full potential with the enhanced sensitivity and multibeam capabilities of SKA and the pathfinders, which will enable simultaneous observations of the target and calibrators. Our demonstration indicates that the 10 micro-arcseconds goal of astrometry at 1.6GHz using VLBI with SKA is feasible using the MultiView technique.

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Section: Discussionmentioning

confidence: 82%

MultiView High Precision VLBI Astrometry at Low Frequencies

Rioja

Dodson

Orosz

et al. 2017

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“…Astrometric terms in pulsar timing models are covariant with red noise in timing data that arises from fluctuations in the pulsar spin-down and/or propagation delays through the ISM that are not completely captured in the pulsar ephemeris. As shown in Deller et al (2016) and Madison et al (2013), red noise can lead to substantial errors in the values and underestimates of the uncertainty for timing-derived parameters. These errors are especially large for unrecycled pulsars with surface field strengths ∼ 10 11 -10 13 G, but are present at some level for all pulsars.…”

Section: Comparison To Timing Astrometrymentioning

confidence: 99%

“…Overall, Figure 16 shows that although for MSPs in some cases the timing measurements of proper motion parameters are comparable to the accuracy of VLBI measurements, the actual values can differ significantly between PTAs. As discussed in Deller et al (2016), there could be multiple explanations, such as contamination by annual DM variations, systematic instrumental noise, the use of different versions of Solar System ephemeris (SSE), or including different levels of noise modelling in the timing solutions. Arzoumanian et al (2018) find the effect of using a different SSE on the proper motion to be on the order of 10 µas yr −1 or less, which is insignificant compared to the current uncertainty levels.…”

Section: Comparison To Timing Astrometrymentioning

confidence: 99%

Microarcsecond VLBI Pulsar Astrometry with PSRπ II. Parallax Distances for 57 Pulsars

Deller

Goss

Brisken³

et al. 2019

ApJ

Self Cite

155

139

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We present the results of PSRπ, a large astrometric project targeting radio pulsars using the Very Long Baseline Array (VLBA). From our astrometric database of 60 pulsars, we have obtained parallaxbased distance measurements for all but 3, with a parallax precision that is typically ∼45 µas and approaches 10 µas in the best cases. Our full sample doubles the number of radio pulsars with a reliable ( 5σ) model-independent distance constraint. Importantly, many of the newly measured pulsars are well outside the solar neighborhood, and so PSRπ brings a near-tenfold increase in the number of pulsars with a reliable model-independent distance at d > 2 kpc. Our results show that both widelyused Galactic electron density distribution models contain significant shortcomings, particularly at high Galactic latitudes. When comparing our results to pulsar timing, two of the four millisecond pulsars in our sample exhibit significant discrepancies in their proper motion estimates. With additional VLBI observations that extend our sample and improve the absolute positional accuracy of our reference sources, we will be able to additionally compare pulsar absolute reference positions between VLBI and timing, which will provide a much more sensitive test of the correctness of the solar system ephemerides used for pulsar timing. Finally, we use our large sample to estimate the typical accuracy attainable for differential VLBA astrometry of pulsars, showing that for sufficiently bright targets observed 8 times over 18 months, a parallax uncertainty of 4 µas per arcminute of separation between the pulsar and calibrator can be expected.

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“…showing clear rapid orbital decay consistent with general relativity prediction due to gravitational wave radiation. White dwarfs have been identified as companions to millisecond pulsars [64][65][66][67][68][69][70][71][72][73][74][75][76] . Ref.…”

Section: Dzsmentioning

confidence: 99%

White Dwarf Stars

Romero

Pelisoli

Ourique

2017

Int. J. Mod. Phys. Conf. Ser.

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White dwarf stars are the final stage of most stars, born single or in multiple systems. We discuss the identification, magnetic fields, and mass distribution for white dwarfs detected from spectra obtained by the Sloan Digital Sky Survey up to Data Release 13 in 2016, which lead to the increase in the number of spectroscopically identified white dwarf stars from 5 000 to 39 000. This number includes only white dwarf stars with log g ≥ 6.5, i.e., excluding the Extremely Low Mass white dwarfs, which are necessarily the byproduct of stellar interaction.

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MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSRπ. I. TWO BINARY MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS

Cited by 38 publications

References 48 publications

MultiView High Precision VLBI Astrometry at Low Frequencies

MultiView High Precision VLBI Astrometry at Low Frequencies

Microarcsecond VLBI Pulsar Astrometry with PSRπ II. Parallax Distances for 57 Pulsars

White Dwarf Stars

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