Abstract
We have learned recently that the inner halo of the Milky Way contains a kinematically coherent component (Gaia-Enceladus) from a significant merger 10 Gyrs ago. By contrast the inner (defined to exclude the Magellanic Stream) halo contains no similar intruder stellar population of billion year age. The tracer we use to set the corresponding upper limit is Gaia asymptotic giant branch stars, rather than Gaia kinematics. The primary sample is drawn from Gaia DR2 with SkyMapper photometry. This is supplemented with PanSTARRS and 2MASS photometry. As the Gaia mission proceeds, a star formation history in the galactic halo should emerge.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Abraham, R., et al.: IAU Symp. 321, 137 (2017)
Arenou, F., et al.: Astron. Astrophys. 616, 17 (2018)
Brown, T., et al.: Astrophys. J. 685, L121 (2008)
Carollo, D., et al.: Astrophys. J. 859, L7 (2018)
Chen, S., et al.: Astrophys. J. 867, 132 (2018a)
Chen, Y., et al.: ASP Conf. 514, 57 (2018b)
Ferguson, A.: IAU Symp. 334, 43 (2018)
Frogel, J., Persson, S.E., Cohen, J.: Astrophys. J. 239, 495 (1980)
Girardi, L.: Astron. Nachr. 337, 871 (2016)
Girardi, L., et al.: Astron. Astrophys. 422, 205 (2004)
Helmi, A., et al.: Nature 563, 43 (2018)
Kaiser, N., et al.: SPIE 77330E (2010)
Lawrence, G.: Honours thesis, Swinburne Univ. (2018)
Li, T., et al.: AAS 233, 12904 (2018)
Majewski, S., et al.: Astron. J. 118, 1709 (1999)
Malhan, K., et al.: Mon. Not. R. Astron. Soc. 481, 3442 (2018)
Mould, J.: Publ. Astron. Soc. Aust. 30, 27 (2014)
Mould, J., et al.: Publ. Astron. Soc. Aust. 35, 1 (2018)
Reid, I.N., et al.: Astrophys. J. 348, 98 (1990)
Renzini, A.: In: Proc. Saas Fee Conf. Advanced Stages in Stellar Evolution, Geneva Obs., Geneva (1977)
Renzini, A., Buzzoni, A.: In: Chiosi, C., Renzini, A. (eds.) The Spectral Evolution of Galaxies, p. 199. Reidel Publishing, Dordrecht (1986)
Rizzi, L., et al.: Astrophys. J. 661, 815 (2007)
Rood, R.: Astrophys. J. 177, 681 (1972)
Saremi, E., et al.: IAU Symp. 344 (2018). arXiv:1812.09725
Schneider, D., Gunn, J., Hoessel, J.: Astrophys. J. 264, 337 (1983)
Schlegel, D., et al.: Astrophys. J. 500, 525 (1998)
Skrutskie, M., et al.: Astron. J. 131, 1163 (2006)
Shipp, N., et al.: Astrophys. J. 862, 114 (2018)
Torrealba, G., et al.: (2018). arXiv:1808.04082
Williams, B., et al.: Astrophys. J. 846, 145 (2017)
Wolf, C., et al.: Publ. Astron. Soc. Aust. 35, 010 (2018)
Author information
Authors and Affiliations
Corresponding author
Additional information
Publisher’s Note
Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Appendix
Appendix
Antlia 2 is a diffuse dwarf galaxy discovered using a Gaia kinematic filter (Torrealba et al. 2018). Such a filter can be added to a query such as the one in Sect. 2.1 and for a radius of 0.63 degrees around the centre of Antlia 2, requiring \(\pi < 0.1\) mas, PMRA\((\cos\delta ) > -1.5\) mas/yr and |PMDEC\(| < 1.5\) mas/yr yields the CMD in Fig. A.1.
Kinematically filtered CMD for Antlia 2 with close to zero parallax and proper motion. The I mag is on the Cousins system. The sloping line is the TRGB of Rizzi et al. (2007), moved to apparent distance modulus 20.5 plus \(A_{I} = 0.3\) mag. A few stars rise above that TRGB in luminosity
The reddening of Antlia 2 is E(B-V) = 0.16 mag according to Schlegel et al. (1998). The red giant branch is clearly seen in the SkyMapper-Gaia photometry and is not seen in a control sample annulus 1 degree from Antlia 2. Evidently, Antlia 2 is closer to 110 kpc away than the 129.4 ± 6.5 kpc measured by Torrealba et al.
Rights and permissions
About this article
Cite this article
Mould, J. The intermediate age population of the Galactic halo. Astrophys Space Sci 364, 42 (2019). https://doi.org/10.1007/s10509-019-3533-0
Received:
Accepted:
Published:
DOI: https://doi.org/10.1007/s10509-019-3533-0