We compare the stellar motion around a spiral arm created in two different scenarios, transient/co-rotating spiral arms and density-wave-like spiral arms. We generate Gaia mock data from snapshots of the simulations following these two scenarios using our stellar population code, SNAPDRAGONS, which takes into account dust extinction and the expected Gaia errors. We compare the observed rotation velocity around a spiral arm similar in position to the Perseus arm, and find that there is a clear difference in the velocity features around the spiral arm between the co-rotating spiral arm and the density-wave-like spiral arm. Our result demonstrates that the volume and accuracy of the Gaia data are sufficient to clearly distinguish these two scenarios of the spiral arms

Cropper, M

Grand, RJJ

Hunt, JAS

Kawata, D

Pasetto, S

Siebert, A

UCL Discovery

arXiv:1502.03570v1  [astro-ph.GA]  12 Feb 2015Title : will be set by the publisherEditors : will be set by the publisherEAS Publications Series, Vol. ?, 2015STELLAR MOTION AROUND SPIRAL ARMS: GAIA MOCKDATADaisuke Kawata1, Jason A.S. Hunt1, Robert J.J. Grand2, 3, ArnaudSiebert4, Stefano Pasetto1 and Mark Cropper1Abstract. We compare the stellar motion around a spiral arm cre-ated in two different scenarios, transient/co-rotating spiral arms anddensity-wave-like spiral arms. We generate Gaia mock data from snap-shots of the simulations following these two scenarios using our stellarpopulation code, SNAPDRAGONS, which takes into account dust extinc-tion and the expected Gaia errors. We compare the observed rotationvelocity around a spiral arm similar in position to the Perseus arm, andfind that there is a clear difference in the velocity features around thespiral arm between the co-rotating spiral arm and the density-wave-likespiral arm. Our result demonstrates that the volume and accuracy ofthe Gaia data are sufficient to clearly distinguish these two scenariosof the spiral arms.1 IntroductionSince the 1960s, the most widely accepted explanation of the spiral arms hasbeen that these features are wave structures, i.e. the density-wave scenario, androtating rigidly (a constant pattern speed) with a different speed from those ofthe stars (Lin and Shu, 1964). However, recent observations of external galaxiesshow evidence against long-lived spiral arms with a constant pattern speed. Forexample, using the modified Tremaine-Weinberg method, Merrifield et al. (2006)suggested a radially decreasing pattern speed for the spiral arms in NGC 1068.1 Mullard Space Science Laboratory, University College London. Dorking, Surrey, RH5 6NT,UK2 Heidelberger Institut fu¨r Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidel-berg, Germany3 Zentrum fu¨r Astronomie der Universita¨t Heidelberg, Astronomisches Recheninstitut, Mo¨nchhofstr.12-14, 69120 Heidelberg, Germany4 Observatoire Astronomique, Universite´ de Strasbourg, CNRS, 11 rue de l’universite´ 67000Strasbourg, Francec© EDP Sciences 2015DOI: (will be inserted later)2 Title : will be set by the publisherAlso, by combining Hα imaging and Swift/UV OT Near-Ultraviolet (NUV) data,Ferreras et al. (2012) distinguished the regions with ongoing star formation andthe regions with star formation a few hundred million years ago in the grand-designspiral galaxy, M100. Contrary to the expectation from the density-wave theory,no offset was found between these two regions. The same conclusion was reachedin Foyle et al. (2011) for different galaxies.The problem is also evident on the theoretical side by using N-body simula-tions. Even with the recent high-resolution numerical simulations not a singleN-body simulation is able to reproduce a long-standing spiral arm feature as sug-gested by the density-wave scenario (e.g Sellwood, 2011; Dobbs and Baba, 2014).Grand et al. (2012a,b) demonstrated that the spiral arm was rotating with thesame speed as the stars, i.e. co-rotating, at every radii, and therefore winding (seealso Roca-Fa`brega et al., 2013). Still, in each snapshot, the spiral arms are alwaysapparent, and the spiral arms are constantly forming and disrupting, i.e. recur-rent, with a lifetime of about 100 Myr. Although co-rotating spiral arms lead tothe winding-dilemma, Grand et al. (2013) demonstrated that the spiral arms weredisrupted before they wound up completely, and the pitch angle of the spiral armscorrelated with the shear rate of the disc, as observed (e.g. Seigar et al., 2006).Interestingly, the winding nature of the spiral arms seen in N-body simulations cannaturally explain the observed scatter in the correlation between the pitch angleand the shear rate (see Grand et al., 2013, for more thorough discussion).The Milky Way is a (barred) spiral galaxy which we can observe in great detail.The influence of the spiral arms on the stellar motion has also been measuredand compared with the models (e.g. Ferna´ndez et al., 2001; Siebert et al., 2012;Faure et al., 2014). The European Space Agency (ESA) Gaia mission will produceaccurate positions and velocities for over a billion stars in the Milky Way, and themajority of them are the disk stars. The Gaia data will provide the opportunity forastronomers to observe in great detail how the stars are moving around the spiralarms in a spiral galaxy, and should provide decisive constraints on the differentspiral arm scenarios.2 Stellar motion around the transient/co-rotating spiral armsThe density enhancement of the co-rotating spiral arms causes an efficient radialmigration for both stars and gas (Grand et al., 2015), because the stars cannotpass or be passed by the spiral arm. For example, the stars behind the spiral armare accelerated by the potential of the spiral arm, and their guiding centre movesoutwards. Because they are rotating with the same speed as the spiral arm, theystay behind the spiral arm and keep being accelerated. Grand et al. (2014) showedthat the stars migrating outward are always behind the spiral arm and at apo-centre phase, i.e. rotating slower than the circular velocity at that radius, while thestars migrating inwards are in the front of the spiral arm and at peri-centre phase.Hunt et al. (2015) generated star samples from an N-body/smoothed particle hy-drodynamics simulation of a Milky Way-sized barred disk galaxy in Kawata et al.(2014) using SNAPDRAGONS (Stellar Numbers And Parameters Determined Rou-Kawata et al.: Stellar Motion around Spiral Arms 3Fig. 1. Galactic rotation velocity distribution of the stars (V < 16 mag) generated withSNAPDRAGONS from the particles in the Galactic longitude of 85 < l < 95 deg and latitudeof −5 < b < 5 deg in an N-body simulation which shows the transient/co-rotating spiralarm (Left) and a test particle simulation of Faure et al. (2014) where the density-wave-like rigidly rotating spiral arm is assumed (Right). Red (blue) line shows the kerneldensity estimation of the rotation velocity distribution of stars behind (in the front of)the spiral arm which is about 4 kpc away from the observer. The vertical dotted lineindicates the circular velocity. Note that the extinction and the expected end-of-missionGaia errors are included.tinely And Generated Observing N-body Systems). SNAPDRAGONS generates thestellar samples taking into account the metallicity and age of a star particle, andproduces the catalogue of stars which are observed from the assumed observerposition, taking into account an empirical 3D extinction (Sharma et al., 2011)and the expected Gaia errors (using the updated version of Romero-Go´mez et al.,2015). Hunt et al. (2015) showed that Gaia has sufficient accuracy to detect thedifference in the velocity distribution behind and in the front of the Perseus arm.3 Transient/co-rotating spiral arms vs. density-wave-like spiral armsTo compare with the stellar motion around the spiral arm in the N-body simulationin Hunt et al. (2015), we also made mock Gaia data using the 3D test particlesimulation data with rigidly rotating, density-wave-like, spiral arms in Faure et al.(2014). Fig. 1 shows the rotation velocity distribution of the stars behind and in thefront of the arm at the Galactic longitude, l = 90 deg, for the N-body simulation(left) and the test particle simulation (right). The position of the observer is set sothat there is a spiral arm at the similar distance to the Perseus arm at l = 90 deg.We consider only the stars with V < 16 mag for which Gaia RVS will produce theaccurate line-of-sight velocity and the rotation velocities will be measured withreasonably high accuracy.In the left panel of Fig. 1, the peak rotation velocity for stars behind thetransient/co-rotating spiral arm is slower than the circular velocity, and the starsin the front of the spiral arm shows a broader distribution. No such differenceis observed in the right panel of the results of the density-wave-like spiral arm.4 Title : will be set by the publisherThis demonstrates that the rotation velocity distribution behind the transient/co-rotating spiral arm in the N-body simulation is different from that in front of thespiral arm, and this is clearly different from the density-wave-like spiral arm inthe test particle simulation. This result also demonstrates that the accuracy ofGaia data is superb, and Gaia will provide enough information to trace the stellarmotion on both sides of the Perseus spiral arm. In transient/co-rotating spiralarms in N-body simulations, the difference in the velocity distribution is expectedto be observed at every radius (Kawata et al., 2014). We can therefore carry outsimilar analysis to Fig. 1 at different radii, i.e. different longitudes, and directlycompare with the Gaia data once they become publicly available. The Gaia datashould therefore be able to distinguish between these two different scenarios of thespiral arms.ReferencesDobbs, C. and Baba, J.: 2014, PASA 31, 35Faure, C., Siebert, A., and Famaey, B.: 2014, MNRAS 440, 2564Ferna´ndez, D., Figueras, F., and Torra, J.: 2001, A&A 372, 833Ferreras, I. et al.: 2012, MNRAS 424, 1636Foyle, K. et al.: 2011, ApJ 735, 101Grand, R. J. J., Kawata, D., and Cropper, M.: 2012a, MNRAS 421, 1529Grand, R. J. J., Kawata, D., and Cropper, M.: 2012b, MNRAS 426, 167Grand, R. J. J., Kawata, D., and Cropper, M.: 2013, A&A 553, A77Grand, R. J. J., Kawata, D., and Cropper, M.: 2014, MNRAS 439, 623Grand, R. J. J., Kawata, D., and Cropper, M.: 2015, arXiv:1410.3836, MNRASin pressHunt, J. A. S. et al.: 2015, arXiv:1501.01969, submitted to MNRASKawata, D. et al.: 2014, MNRAS 443, 2757Lin, C. C. and Shu, F. H.: 1964, ApJ 140, 646Merrifield, M. R., Rand, R. J., and Meidt, S. E.: 2006, MNRAS 366, L17Roca-Fa`brega, S. et al.: 2013, MNRAS 432, 2878Romero-Go´mez, M. et al.: 2015, MNRAS 447, 218Seigar, M. S., Bullock, J. S., Barth, A. J., and Ho, L. C.: 2006, ApJ 645, 1012Sellwood, J. A.: 2011, MNRAS 410, 1637Kawata et al.: Stellar Motion around Spiral Arms 5Sharma, S. et al.: 2011 ApJ 730, 3Siebert, A. et al.: 2012, MNRAS 425, 2335

Stellar Motion around Spiral Arms: Gaia Mock Data

http://discovery.ucl.ac.uk/1485047/1/kawata_stellar_motion_around_spiral_arms.pdf

Stellar Motion around Spiral Arms: Gaia Mock Data

Abstract

Similar works

Full text

Available Versions

UCL Discovery