Constraining the thick disc formation scenario of the Milky Way

Abstract

Aims. More than 30 years after its discovery, the thick disc of the Milky Way is not fully explored. We examine the shape of the thick disc in order to gain insight into the process of its formation. Methods. The shape of the thick disc is studied in detail using photometric data at high and intermediate latitudes from SDSS and 2MASS surveys. We adopted the population synthesis approach using an approximate Bayesian computation -Markov chain Monte Carlo (ABC-MCMC) method to determine the potential degeneracies in the parameters that can be caused by the mixing with the halo and the thin disc. We characterised the thick-disc shape, scale height, scale length, local density, and flare, and we investigated the extent of the thick-disc formation period by simulating several formation episodes. Results. We find that the vertical variation in density is not exponential, but much closer to a hyperbolic secant squared. Assuming a single formation epoch, the thick disc is better fitted with a sech 2 scale height of 470 pc and a scale length of 2.3 kpc. However, if one simulates two successive formation episodes, which mimicks an extended formation period, the older episode has a higher scale height and a longer scale length than the younger episode, which indicates a contraction during the collapse phase. The scale height decreases from 800 pc to 340 pc, the scale length from 3.2 kpc to 2 kpc. The likelihood is much higher when the thick disc formation extends over a longer period. We also show that star formation increases from the old episode to the young and that there is no flare in the outskirt of the thick disc during the main episode. We compare our results with formation scenarios of the thick disc. During the fitting process, the halo parameters are determined as well. If a power-law density is assumed, it has an exponent of 3.3 and an axis ratio of 0.7. Alternatively, a Hernquist shape would have an exponent of 2.76, an axis ratio of 0.77, and a core radius of 2.1 kpc.The constraint on the halo shows that a transition between an inner and outer halo, if it exists, cannot be at a distance shorter than about 30 kpc, which is the limit of our investigation using turnoff halo stars. Finally, we show that extrapolating the thick disc towards the bulge region explains well the stellar populations observed there that there is no longer need to invoke a classical bulge. Conclusions. The facts that the thick-disc episode lasted for several billion years, that a contraction is observed during the collapse phase, and that the main thick disc has a constant scale height with no flare argue against the formation of the thick disc through radial migration. The most probable scenario for the thick disc is that it formed while the Galaxy was gravitationally collapsing from well-mixed gas-rich giant clumps that were sustained by high turbulence, which prevented a thin disc from forming for a time, as proposed previously. This scenario explains well the observations in the thick-disc region and in the bulge region.

Evolution over time of the Milky Way’s disc shape

“…As it is still undergoing testing, its use will be deferred to future studies. New revisions concerning the thick disc and halo populations have been discussed by Robin et al (2014). We do not make use here of the new characteristics of the thick disc and halo, but they should affect the present study only very marginally.…”

“…To estimate the number of parameters and the effective improvement in the χ 2 , we compute the Bayesian information criterion (BIC; Schwarz et al 1978). We follow the recipes of Robin et al (2014) first computing the reduced likelihood (Lr, Eq. (16)) for a binomial statistics (Bienaymé et al 1987), as described below:…”

Kinematics of the local disk from the RAVE survey and the Gaia first data release

“…For the thick-disk and halo population, the simulations are based on Robin et al (2014), where the thick-disk structural and age parameters have been constrained together with the halo from color-magnitude diagrams fitting to SDSS and 2MASS photometry. We adopt here the thick-disk model shape B (secant squared in z gal ) and a Hernquist halo with a core radius of 5.17 kpc and an axis ratio of 0.776.…”

“…The relative continuity (or lack of clear separation) of the two disk populations, when no elemental abundances are available, has been the source of misunderstanding and apparent inconsistency between various analyses. With the help of the alpha-element abundance ratio it can be easier to analyze, since it has been shown in local samples (Adibekyan et al 2013) and more distant samples (Hayden et al 2014 According to Robin et al (2014), the scale length and scale height change from the beginning (12 Gyr ago) to the end of the phase (10 Gyr ago) because of contraction. Hence we expect that the velocity ellipsoid and rotation velocity show a similar behavior.…”

“…They used parameters from an older stellar population model (Robin et al 2003) introduced in the Galaxia (2017) model Sharma et al (2011). Similar density laws are assumed for the thin and thick disks, but we have shown in Robin et al (2014) that the parameters of the thick disk in Robin et al (2003) are not accurate, although the impact of this assumption on their analysis might be minor. They tested distributions in velocities to be Gaussian or Shu distributions, and used the asymmetric formula proposed by Bovy et al (2012).…”