Issue 
A&A
Volume 584, December 2015



Article Number  A120  
Number of page(s)  20  
Section  Galactic structure, stellar clusters and populations  
DOI  https://doi.org/10.1051/00046361/201526203  
Published online  02 December 2015 
The evolution of streams in a timedependent potential^{⋆}
Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
email: buist@astro.rug.nl
Received: 27 March 2015
Accepted: 17 June 2015
We study the evolution of streams in a timedependent spherical gravitational potential. Our goal is to establish what are the imprints of this time evolution on the properties of streams as well as their observability. To this end, we have performed a suite of testparticle experiments for a host system that doubles its mass during the integration time and for a variety of initial conditions. In these experiments we found that the most striking imprint is a misalignment of ~10° in the angular location of the apocentres of the streams compared to the static case (and to the orbit of the centre of mass), which only becomes apparent for sufficiently long streams. We have also developed an analytic model using actionangle variables which allows us to explain this behaviour and to identify the most important signature of time evolution, namely a difference in the slope defined by the distribution of particles along a stream in frequency and in angle space. Although a difference in slope can arise when the presentday potential is not correctly modelled, this shortcoming can be bypassed because in this case, streams are no longer straight lines in angle space, but depict a wiggly appearance and an implausible energy gradient. The difference in slope due to time evolution is small, typically ~10^{2} and its amplitude depends on the growth rate of the potential, but nonetheless we find that it could be observable if accurate fullspace information for nearby long streams is available. On the other hand, disregarding this effect may bias the determination of the presentday characteristics of the potential.
Key words: dark matter / Galaxy: halo / Galaxy: kinematics and dynamics / Galaxy: structure / galaxies: evolution
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
1. Introduction
Throughout the history of the Milky Way and in the context of the Λ cold dark matter cosmogony, many dwarf galaxies must have been disrupted, leaving behind stellar streams (Helmi & White 1999). Especially the Galactic halo probably contains many such relics of this assembly history (Helmi 2008).
Tidal streams were predicted for the first time in the seminal work of Toomre & Toomre (1972) who simulated the interactions of two galaxies. LyndenBell & LyndenBell (1995) and Johnston et al. (1996) put forward the idea of tidal streams lurking in the Galactic halo, merely a few years after the discovery of the Sagittarius dSph by Ibata et al. (1994). Streams and debris from the Sagittarius stream were found several years later by Ivezić et al. (2000), Yanny et al. (2000), Ibata et al. (2001b), and a fullsky view of the Sagittarius stream was provided by Majewski et al. (2003). Other examples are the globular cluster streams (Grillmair et al. 1995), such as Palomar 5 (Odenkirchen et al. 2001) and NGC 5466 (Grillmair & Johnson 2006). A wealth of new streams have been found in the Sloan Digital Sky Survey (see e.g. Grillmair & Dionatos 2006), in the “Field of Streams” (Belokurov et al. 2006). Streams have also been found with other galaxies (MartínezDelgado et al. 2010; Martin et al. 2014), most notably around M31 (Ibata et al. 2001a).
On the modelling side, much effort has been put into understanding the dynamics of streams and using these to infer the Galactic potential. Stream stars follow trajectories that are very similar to those of their progenitors (Jin & LyndenBell 2007; Binney 2008), albeit slightly offset. The evolution of streams is relatively simple in actionangle coordinates (Helmi & White 1999; Tremaine 1999). Furthermore, streams appear as distinct clumps in integrals of motion space (Helmi et al. 1999; Helmi & de Zeeuw 2000), and they show the highest coherence in the true (underlying) potential. This can be used to constrain its characteristic parameters (Peñarrubia et al. 2012; Sanderson et al. 2014). The alignment of the angles and orbital frequencies can aid in determining the potential, as proposed by Sanders & Binney (2013a).
The current cosmological model predicts significant evolution in the mass content of galaxies and of their dark matter haloes through cosmic time (Springel et al. 2005). This evolution may be directly measurable using stellar streams, given their sensitivity to the gravitational potential in which they are embedded (Johnston et al. 1999; Eyre & Binney 2009; PriceWhelan et al. 2014; Bonaca et al. 2014). A first study was presented by Peñarrubia et al. (2006), who concluded that there are no discernible effects of evolution on the distribution of streams in the space of angular momenta and energy because they only reflect the potential at the present day. However, Gómez & Helmi (2010) found that the structure of streams in frequency space does depict longlasting signatures of time evolution. Bonaca et al. (2014) also found several biases when they attempted to derive the characteristic parameters of a time dependent potential using streams. They attributed these biases partly to the time evolution of the potential in their simulations.
In the coming decade, the Gaia satellite (Perryman et al. 2001), successfully launched in 2013, will provide an unprecedented vast and detailed view of our Galaxy. With the correct understanding of streams, Gaia will allow us to address the assembly history of our Milky Way. This is the main motivation of this paper. Our goal is to establish what kinds of observable imprints remain on the stream properties and how to use them in recovering the evolutionary path of the Galactic potential. To this end we use the cosmologically motivated growth model of a spherical halo by Buist & Helmi (2014) and follow the evolution of streams both numerically and using the actionangle formalism.
This paper is organised as follows. In Sect. 2 we explain the simulations of streams in a timedependent potential. We analyse the simulations in Sect. 3 and develop an analytic model based on actionangles in the adiabatic regime. This allows us to identify the signature of time evolution on a stream in Sect. 4. In Sect. 5 we explore the prospects of observing this effect. We conclude in Sect. 6.
2. Methodology
To understand the behaviour of streams in timedependent potentials, we take two complementary approaches. We first numerically study the evolution of groups of test particles that initially resemble a satellite galaxy. We then attempt to model this evolution using a formalism based on actionangle variables. In Sect. 2.1 we describe the setup of our numerical experiments, and in Sect. 2.2 we briefly introduce the actionangle variables and their properties.
2.1. Simulation setup
2.1.1. Evolution of the gravitational potential
We modelled the evolution of a timedependent NavarroFrenkWhite potential (Navarro et al. 1997, NFW) using the prescription models from Buist & Helmi (2014). This model gives rise to an insideout smooth growth that well reproduces the average mass accretion history of the MilkyWaysized haloes from the Aquarius simulations (Springel et al. 2008; Wang et al. 2011). An important characteristic of this model is that mass growth is positive at each radius (i.e. there is no inward flow of mass between neighbouring mass shells). The scale radius r_{s} and the scale mass M_{s} (mass enclosed within r_{s}) of such a halo vary according to (1)where z is the redshift, and M_{s,0} and r_{s,0} the scale mass and scale radius at the final time (z = 0, in a cosmology with Ω_{m} = 0.29 and h_{100} = 0.71). We used γ = 2 to grow insideout for an NFW potential (Buist & Helmi 2014). The parameter a_{g} determines the formation epoch, and higher values correspond to more recent formation. We here explore a range of values of a_{g} up to a_{g} = 0.8, which would represent a quite recent formation epoch.
We modelled the evolution of streams in this timedependent potential, but we also studied their behaviour in the static case. To make a fair comparison, we fixed the scale mass and scale radius at the final time to M_{s} = 5 × 10^{11}M_{⊙} and r_{s} = 12 kpc for all our experiments, independent of their time evolution.
2.1.2. Orbits
Orbital properties at the final time.
Fig. 1 Increase of the enclosed mass for several orbits for our timedependent potential with a growth factor of a_{g} = 0.8. The dashed lines show the enclosed mass within the final value of their apocentre. Since the apocentric distances shrink with time, we show the mass enclosed within the timedependent apocentre values with solid lines. The integration time span for the streams is t ~ 7–8 Gyr, and the enclosed mass approximately doubles over this timescale. 

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We placed the satellites on 15 different orbits as listed in Table 1. We chose this number to have a variety in distances, orbital timescales (and hence the degree of adiabaticity), and eccentricity of the streams. The apo and pericentres at the final time were chosen such that the particles spend most of their time in the outer halo and beyond the scale radius of the potential. For a fair comparison of each experiment the final 6D position of the satellite’s centre of mass is the same for the static and timedependent cases. We then integrated the orbits backwards in time for about 7–8 Gyr and the more circular orbits for 6–7 Gyr. This range was chosen to ensure that all orbits are bound at early times in the timedependent case.
We chose to start our orbital integrations when the satellite’s centre of mass was at its first pericentre to represent the first interaction with the Galaxy. This implies that the various orbits have slightly different total integration times, but these only differ up to a maximum of 0.5 Gyr. Within this integration time, the enclosed mass within a fixed radius increases on average with more than a factor 2 in our halo, as seen in Fig. 1. The actual orbits experience a somewhat smaller increase in enclosed mass because they respond to the halo growth by shrinking slowly.
2.1.3. Progenitors
We distributed the particles in the satellites assuming they follow an isotropic Gaussian in position and in velocity space, characterised by dispersions σ_{pos} and σ_{vel}. We used 10 000 particles centred on the centre of mass of the satellite, which was placed on the orbits described previously. We did not include selfgravity in our simulations. We considered three different progenitors, which we called “Carina”, “Sculptor” and “Sagittarius” because they have properties reminiscent of these dwarf spheroidal satellites of the Milky Way (see e.g. Martin et al. 2008; Wolf et al. 2010, see Table 2).
2.2. Actionangle coordinates
2.2.1. Generalities
A particularly useful description of the evolution of streams may be obtained using actionangle coordinates (Goldstein 1950; Helmi & White 1999; Tremaine 1999). In actionangle coordinates, the actions are the momenta and the angles are the coordinates. The actions are integrals of motion that are adiabatic, or in other words, invariant under slow changes of the host potential.
In this section, we only work with a timeindependent potential. For a single star, the actions can be found from (2)with p_{i} the conjugate momentum of coordinate q_{i}, and to indicate that we integrate over a full period of coordinate q_{i}. In a spherically symmetric system the actions are the radial, latitudinal and azimuthal actions (J_{r}, J_{θ}, and J_{φ} respectively), and the angles are θ_{r}, θ_{θ}, and θ_{φ}, and represent the phase of the orbit in the r, θ, and φ coordinates, respectively.
For only a few potentials algebraic expressions of the actions can be derived, such as for the isochrone potential (of which the Kepler potential and harmonic oscillator are limiting cases). Typically numerical methods are therefore required to find the actions (Binney & Tremaine 2008). Furthermore, actions are only directly available when the HamiltonJacobi equations are separable, as in the case of spherical and Staeckel potentials (Goldstein 1950; de Zeeuw 1985). In more general axisymmetric and triaxial potentials, approximations to the actions and angles must be used (see e.g. Kaasalainen & Binney 1994; Binney & McMillan 2011; Binney 2012; Sanders & Binney 2014, 2015; Bovy 2014).
Progenitor properties.
Fig. 2 Relation between the coordinates and the angles in the plane of the orbit. The top panel shows that the radial angle θ_{r} increases by 2π in one radial oscillation. In the bottom panel we have plotted φ (red) and θ_{φ} (blue) as functions of θ_{r}. After one radial period, both angles reach the same value 2πΩ_{φ}/ Ω_{r}. 

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Hamilton’s equations for the J_{i} and θ_{i} are (3)and H = H(J) only because the actions are invariant. The Ω_{i} are constants that correspond to the orbital frequencies and also only depend on the J_{i}. The resulting equations of motion for the θ_{i} are (4)with θ_{i}(0) the initial phase of ith coordinate.
To determine the angles, we used a canonical transformation of the second kind W(q,J) (Goldstein 1950; Binney & Tremaine 2008), such that (5)The generating function for the transformation in a spherical potential is given by (adapted from Binney & Tremaine 2008) (6)where the integration is along the trajectory of a particle in phase space. We note that the three parts of the generating function are indefinite versions of the action integrals without a factor of 2π, and each increases therefore by 2πJ_{i} in their corresponding periods 2π/ Ω_{i}. This equation has an algebraic expression in the case of an isochrone potential and has to be solved numerically otherwise. For the full integrals needed to compute θ_{i} in a spherical potential we refer to Appendix A.
Fig. 3 Distribution in action (left), frequency (second panel) and angle space (right) for particles in a stream, and centred on the centre of mass of the progenitor system. The colours represent the energy gradient, where red is for the trailing and green for the leading arms. 

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In Fig. 2 we show an example of how the radial and azimuthal angles (θ_{r} and θ_{φ}) are related to the radial and azimuthal coordinates (r and φ) in the orbital plane. Since W_{φ} = φJ_{φ} and using Eqs. (5) and (6)^{1}(7)The term has a nonsecular oscillation with frequency Ω_{r} and vanishes at apo and pericentre (θ_{r} = {0, ± π}). The secular behaviour of φ and θ_{φ} with time is therefore the same, as can also be seen in Fig. 2.
2.2.2. Streams in actionangle coordinates: timeindependent case
A stream is created when particles drift away from the progenitor, which means we should look at the relative phase with respect to the progenitor centre of mass. For example, the relative azimuthal phase of the kth particle is (8)where is the separation in angles at the initial time, and where the second line corresponds to the case in which the progenitor is small and the stream has evolved for a sufficiently long time.
The depends on the distribution in action space , such that a broad action spread results in a wide range of frequencies. This implies that larger progenitors generate longer streams than smaller ones if integrated for the same amount of time.
In Fig. 3 we show the structure of a stream in actionangle coordinates for the timeindependent case. The colours represent the energy gradient, such that green represents the leading tail and red the trailing tail. The left panel shows the action distribution, which depends both on the initial conditions σ_{pos} and σ_{vel} and on the initial orbit^{2}. This distribution also remains invariant in time in an adiabatically evolving potential. The secondleft panel of shows the structure in frequency space, while the third corresponds to angle space. Since angles are 2π periodic variables, in the right most panel we show the angles modulo 2π. The different streaks signify the number of radial and azimuthal wraps the stream has. We note that the slope of the lines in frequency and in angle space are the same in this timeindependent potential (Sanders & Binney 2013a) when the initial spread in angles can be neglected^{3}: (9)This directly shows why all particles are distributed along straight lines with the same slope in angle and in frequency space.
3. Analysis of the testparticle simulations
Fig. 4 Streams from three progenitor sizes for each of the 15 orbits evolved in the timedependent a_{g} = 0.8 potential. The left, middle, and right panels correspond to the “Carina”, “Sculptor”, and “Sagittarius”like progenitors, respectively (see Table 2 for their properties). Particles in green are more bound to the host galaxy (leading arm), while those in red are less bound (trailing arm) than the progenitor. The dashed curves are the progenitor orbits evolved in today’s potential, with the green integrated forward in time for the leading arm and red backwards for the trailing arm. The current position of the progenitor is indicated with a red cross. 

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Fig. 5 Radial vs. angular distribution of particles in the orbital plane for experiment O7 for the different progenitors in the timedependent case. The dashed curves show the orbit of the centre of mass of the system integrated long enough to roughly reproduce the lengths of the streams. The variations in the apocentric distances are a reflection both of time evolution and of the energy gradient present along a stream. The difference in angular location of the apocentre, on the other hand, is a clear imprint of time evolution, as can be seen by comparing to e.g. Fig. 7. 

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Fig. 6 Streams from the Carina progenitor in the evolving and in the nonevolving potential. The streams in the left and centre have the same initial distribution in configuration and velocity space. Those in the right panels have the same initial actionangle distribution as the timeevolving potential (middle panel), but are evolved in a static potential. The colour coding is the same as in the previous figure. The streamorbit misalignment can be seen by looking at the azimuthal angle of the petals starting from one radial period away from the progenitor, whose position is indicated with a red cross. 

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Fig. 7 Radial vs. angular distribution of particles in the orbital plane for experiment O7 for the Carinalike progenitor in the static case (left), timedependent case (middle), and static case with the same initial actionangle distribution as in the middle panel. The dashed curves show the orbit of the centre of mass of the system integrated in the presentday potential for the left and right panels, and in the evolving potential for the middle panel. For the static cases, the variations in the apocentric distances are a reflection of the energy gradient present along the stream, while a second effect is present in the middle panel because of time evolution. In this case, the difference in angular location of the apocentre is also much more pronounced and systematically increases for older wraps. 

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Fig. 8 Actionspace distributions for a sample of four streams from Fig. 6, measured with respect to the centre of mass of the progenitor at the final time. The colours of the particles represent the energy gradient, such that green is the leading arm and red the trailing arm. In the static cases, the initial and final distributions coincide exactly, but in the timedependent case there can be small deviations if the orbit is not in the adiabatic regime, as can be seen by comparing the middle and right panels for orbits O11 and O15. The left panels show a smaller spread because the timedependent cases start farther outwards and in an initially much lighter potential. 

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The results of the simulations for the three progenitors on the various orbits for the timedependent potential with growth factor a_{g} = 0.8 are shown in Fig. 4. The colour coding indicates the leading (green) and trailing (red) arms of the stream. For comparison we have overplotted the orbit of the progenitor integrated forward and backwards in time in the presentday potential. The time of integration for that orbit is between 1 to 3 Gyr and is chosen to roughly match the length of the corresponding stream. Note that this is much shorter than the time of integration of the particles that form the stream, which is approximately 8 Gyr.
Figure 4 clearly shows that larger progenitors give rise to longer and wider streams. The smaller (Carina) progenitor generates thin, short streams, which makes the separate loops of the stream easily recognizable by eye, while the streams from the larger progenitors, depending on the specific orbit considered, are wider and longer, much more phase mixed, and sometimes difficult to discern. As we show below, a clear imprint of the time evolution of the potential is apparent in the angular location and in the variation of the maximum distance of each “petal” of a stream (the latter being related to both the shrinking of the progenitor’s orbit because of mass growth and to the energy gradient along a stream). This effect is more easily discernible for heavier progenitors since they produce more loops, that is, longer streams, as can be seen in Fig. 5. On the other hand, thinner streams have the advantage that they depict their mean orbit much more clearly, which is the reason we mainly focus on the “Carina” progenitor in what follows.
The differences in the evolution for timedependent and static potentials are shown in Figs. 6 and 7 for the Carinalike progenitor, depicted as before on the orbital plane of the progenitor. We note that in all cases the stream in the timedependent potential is longer than in the static case, as can be seen by comparing the left and middle panels.
The length of a stream depends both on the orbital period and on the initial extent in phase and configuration space of the progenitor. In the timedependent potential the enclosed mass at initial times is lower, and the progenitor starts farther out. This results in lower orbital frequencies, or longer periods. Since the rate of divergence of particles in a stream in a spherical potential is proportional to (t/P)^{2} ∝ (Ωt)^{2} (Helmi & White 1999), this would imply that streams should actually be shorter for a fixed integration time t. However, in a timedependent potential the spread in actions (or integrals of motion such as the energy) is broader for given initial σ_{pos} and σ_{vel} (see Fig. 8).
For an initially “compact” ensemble of particles, we may use a linear transformation between actionangle coordinates and Cartesian coordinates to derive the initial spread in actionangle space: (10)where the elements of the transformation matrix T will depend on second derivatives of the generating function evaluated at the centre of mass of the progenitor (Helmi & White 1999), as described in detail in Appendix B. We see that many of the terms depend on 1/Ω_{r}, which is larger in a shallower potential and farther out in the potential, confirming that the initial spread in actions is greater. Therefore the particles in the progenitor integrated in the evolving potential can spread more and give rise to longer and wider streams.
In our initial setup we took the progenitors to have the same σ_{pos} and σ_{vel}. However, their initial distribution in actionangle space is different for the static and timedependent potentials, as discussed above. This implies that their final distribution in action (or energy) space will also be different. This is shown for the progenitor placed on two of our orbits in Fig. 8. Here we have plotted the distribution at the final time of ΔJ_{r} and ΔL in the top panels for the static (left) and timedependent (middle) potentials for the “Carina”like progenitor.
An alternative is to consider that the particles have the same initial ΔJ_{r} and ΔL, whether they are evolved in a static or timedependent gravitational potential. To establish the effect of such a change in the initial configuration, we set up progenitors with these properties and evolved them in the static potential. The right panels of Fig. 8 show the distribution of particles evolved in the static potential, but set up with the same initial conditions in actionangle space as in the timedependent case. If all orbits were in the adiabatic regime, the middle and right panels should give identical results. However, some of the orbits are not, which can be seen in the streams from orbits O11 and O15, where the action distributions are not exactly the same.
The streams resulting from these different initial conditions evolved in the timeindependent potential are shown in the right panels of Fig. 6 for each of the orbits. As anticipated, the streams in the timedependent potential (middle panels) are now shorter than the streams in the timeindependent potential starting from the new initial conditions. This characteristic is now solely due to the evolution of the potential.
An interesting feature visible in Figs. 6 and 7 that was mentioned earlier is that the streamorbit misalignment differs in the static and evolving cases. For example, as can be seen for experiment O7, the mean orbit traces the stream in the timeindependent case relatively well. On the other hand, it is clear that the angular position of the rosette petal of the stream and the progenitor orbit at one radial period behind (or ahead) are offset from each other. This is apparent in all experiments, to a lesser or greater degree. This offset is systematic, can be as large as 10 degrees, and is a first direct indication of the effect of time evolution on the gravitational potential.
4. Analytic models
4.1. Actionangle coordinates in an adiabatically evolving potential
In this section our aim is to extend the use of actionangles to an adiabatically changing spherical potential. The actionangles are still a valid canonical coordinate system in a timedependent system, but the equations of motion in actionangle coordinates are more complicated, as we show below.
In the models we have considered so far, the gravitational potential is made time dependent by making its characteristic parameters, such as mass and scale, a function of time. Its overall shape or functional form remain the same. Therefore angular momentum is still conserved because of the assumed spherical symmetry, but the radial action J_{r} may vary with time.
For a timedependent potential, the generating function that allows the transformation between Cartesian and actionangle spaces is an explicit function of time (11)where the parameters of the potential are in the vector α. The appropriate Hamiltonian in actionangle coordinates then becomes (12)which is the original Hamiltonian perturbed by the partial time derivative of the generating function (Goldstein 1950, Sects. 11–7). This extra term naturally vanishes in the timeindependent case. The new equations of motion are (13)Compared to the original equations of motion given in Eq. (3), there are a few correction terms that depend on the rate of change of the characteristic parameters of the potential .
Since in general we are interested in the mean increase in the actions and angles, we take an average over one period, where we assume that α changes little over one period (Goldstein 1950; Vandervoort 1961) (14)The three parts of the generating function (W_{r}, W_{θ} and W_{φ}) increase by 2πJ_{i} in the corresponding period T_{i}. This means that each of the W_{i} is a periodic function, and we can do a Fourier expansion (15)However, the whole first term in Eq. (14) vanishes since (16)where we use the Einstein summation convention for the parameters α_{m}. The actions are therefore invariant up to second order. Vandervoort (1961) showed that the actual condition for adiabatic evolution for each of the α_{m} and each of the orbital periods T_{i} is (17)which states that the timescale of change should be much longer than the orbital period.
Fig. 9 Response of the radial action and the radial frequency to a timedependent potential for orbit O7 (Table 1). For this orbit, the action shows a nonsecular oscillation that decreases in amplitude as the rate of change of the potential decreases. The value of Ω_{r} changes significantly with time, and here there are also oscillations that become smaller as the change rate of the potential decreases. The period of the oscillations corresponds with the radial period. The evolution of J_{r} has been quite adiabatic because it oscillates around a limiting value, which is the starting value when the particles were released at pericentre. 

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On short timescales, J_{r} shows a periodic oscillation that decreases in amplitude when the changes in the parameters become smaller, as shown in Fig. 9 for one of our orbits. The final time value of J_{r} returns to the initial value, indicating we are in the adiabatic regime^{4}. In the case of nonadiabaticity, full integration of Eq. (13) is needed to model the behaviour of the system in actionangle space.
In an analogous way as for the actions, we compute the effect for the mean change in the angles (18)where we can exchange the order of the derivatives (19)The result is that only the term dependent on the (evolving) frequency remains (20)The angles as a function of time may be computed from (21)where like in the timeindependent case, θ_{i}(0) is the phase at the initial time. The frequencies Ω_{i}(t) are understood to be the instantaneous frequencies at every time step. Equivalently, we can numerically integrate the orbit in Cartesian coordinates and find θ_{i}(t) from the instantaneous coordinate transformation at all times t using the generating function. The advantage of the actionangle description is that it stresses that the phase angles (modulo 2π) depend on how the frequencies have changed with time.
4.2. Streams in actionangle space
4.2.1. Sensitivity to the gravitational potential
Fig. 10 Angle space of stream O7 (see Table 1) evolved in a timedependent potential, but where the angles have been computed with different (incorrect) parameters. The central panel shows the correct parameters, while r_{s} is changed vertically and M_{s} horizontally by 10% and 30%. The colour coding indicates the energies, with green representing the leading arm (more bound) and red the trailing arm (less bound). 

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Fig. 11 Angle space of streams O11 (top) and stream O1 (bottom) evolved in a timedependent potential, but where the angles have been computed with different (incorrect) parameters. We note that although the distortions in angle space are less pronounced for the more radial orbit O1, the energy gradient (indicated by the colour gradient and coding used before) is not preserved. 

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We have mentioned that if the initial spread in angles is negligible, then the slopes in the angle and frequency spaces should be equal for a static potential (Sanders & Binney 2013b,a), as can be seen from Eq. (8), if computed in the true potential. An example of the distortion in angle space for a stream now evolved in a timedependent potential where the angles (and the energy) were computed using incorrect parameters is shown in Fig. 10 for experiment O7. The central panel corresponds to the parameters in the true (final) potential, while we varied r_{s} in the vertical and M_{s} in the horizontal direction. The parameters in the eight panels around the central panel were changed by only 10%, and even in this case, some deviations from the expected straight lines are visible. When the parameters were changed by as much as 30%, as in the outer panels, the deviations become much more pronounced and are very strong. We note that similar results are found when the stream is evolved in a static potential.
The more incorrect the potential, the more we see wiggles in angle space. Similar distortions are also present in the frequency spaces and action spaces. Furthermore, the energy gradient along the stream is no longer preserved as the parameters of the potential are varied, which implies that the most bound (least bound) particles in the specific trial potential are no longer “found” at the end of the leading tail (trailing tail). Although the streams have a normal appearance in physical space, the coordinate transformation to actionangle space and the computation of the energy are incorrect when the wrong gravitational potential is assumed. This leads to the distorted appearance and broken energy gradient seen in Fig. 10. Clearly, these imprints will only be obvious for sufficiently long streams, that is, those more extended than 2π in angle space.
We note that the distortions in angle space are less pronounced for the panels located along the diagonal that runs from bottom left to top right in Fig. 10, for which the enclosed mass within the orbit is the same for the given M_{s} and r_{s}.
The degree to which these distortions and broken energy gradients manifest also depends on the type of orbit the stream progenitor has followed. This is shown in Fig. 11 for a scale radius that is 70% of the true value and for different scale masses M_{s}. The top panels correspond to experiment O11, which is on a relatively circular orbit of apocentretopericentre ratio of 2, while the experiment in the bottom O1 has a relatively radial orbit, with apocentretopericentre ratio of 18.
4.2.2. Sensitivity to timedependence
In the timedependent potential the exact correspondence between the slopes of the spreads in the frequencies and in the angles is broken, meaning that Eq. (9) is no longer valid. This is because the evolution of Δθ_{φ} and Δθ_{r} depends on integrals over time, that is,(22)(assuming the initial angle spreads are negligible).
In Fig. 12 we compare the lines fitted to the frequency and angle spaces for the stream from orbit O7 in the timedependent and static cases for the correct final potential. The top panel shows that for the timedependent case, the initial slope in frequency space (grey line) is steeper than at the end of the simulation (blue line). This is because the orbit shrinks as the mass increases^{5}. In the timeindependent case we see, as expected, that both lines coincide. Another difference between the static and evolving case is that the streamorbit misalignment changes (compare the green and red dashed lines), which is only caused by the changes in the angle space due to time evolution. The behaviour in angle space (indicated by the red dashed line) may be understood from the fact that the angles’ slope is like a time average of the frequencies’ slope, and is therefore expected to lie between the initial and the final frequency slope as observed. Therefore, a clear signature of time evolution is a difference in the slope derived for the angles and that derived for the frequencies, even if they are computed using the presentday gravitational potential.
We now explore an analytic model to describe the behaviour of the frequency and angle slopes more generally. We may derive the slope in frequency space S(ΔΩ) by making a Taylor expansion in the actions near the centre of mass of the progenitor (Helmi & White 1999) (23)The expansion is done for the kth particle, all terms are evaluated at time t. The derivative is evaluated for the progenitor orbit and we used the Einstein summation convention on the subscript indices. We recall that (24)Working out the frequency spreads, we find The cross terms are second derivatives of the Hamiltonian and therefore symmetric, H_{ij} = H_{ji}. Furthermore, in a spherical potential, the Hamiltonian is only a function of E and L, so that for all j, H_{θj} = H_{φj}^{6}. The evolution of the slope of S(ΔΩ) can then be found from (25)Here is the ratio of the actions and h_{i} the ratio of the Hessians. The Hessians H_{ij} and the Hessian ratios h_{i} are shown in Fig. 13 and are ranked as  H_{rr}  >  H_{φr}  >  H_{φφ} . But most importantly, the resulting ratio h_{r} increases with time, while h_{φ} decreases with time. Assuming that the action ratio remains constant (adiabatic limit), we find from this equation that the slope in frequency space S(ΔΩ) decreases with time.
For the angles of the kth particle we can use the following approximation (26)where we have neglected the initial angle spread and in the last approximation assumed adiabaticity of the actions. Therefore may be evaluated at any time step, although we typically use the values at the final time in our computations.
Fig. 12 Lines fitted to the angle space (red dashed line) and the frequency space (blue line) of stream O7 evolved in a timedependent (top) and static potential (bottom) using the same (correct) final potential. Additionally, the green line shows the track of the progenitor assuming the potential is static (i.e. θ_{cm}(t) = Ω_{cm}(t_{f})t), and the grey line shows the line fitted to the frequency space at the beginning of the simulation. The inset labels show the numerical values of the aperture angle (misalignment) between the stream and the (static) progenitor orbit Ψ_{S, O}, and between the stream in angle and in frequency space Ψ_{Δθ, ΔΩ} (see Eqs. (34) and (35)). 

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We now focus on the slope in angle space. If we define (the timeaveraged Hessian), then The slope in the angles can then be found from (27)Here the q_{i} are the ratios of the Q_{ij}. The ranking of the Q_{ij} and the q_{i} behaves very similarly to that of the H_{ij} and h_{i}, as shown in Fig. 13. In the same manner as for the frequency slope, we infer that S(Δθ) is also a decreasing function of time.
We are now ready to compute the difference between S(Δθ) and S(ΔΩ) by using that the difference between the q_{i} and the h_{i} is small: where the appropriate sign was chosen such that the ϵ_{i} are always positive. We define for computational ease We may expand the inverse of the angle slope T(Δθ)(32)Using Eq. (25) to compute T(Δθ), we can derive the difference of the inverse slopes (33)All the terms in the fraction are positive, and T(ΔΩ) is therefore always greater than T(Δθ). This means that S(Δθ) is always larger than S(ΔΩ), and this difference will increase with time. The longer the system is evolved in a timedependent potential, the larger the difference in slopes becomes with respect to the same final static potential. This also means that streams that fell in at early times will show a stronger signature of the separation between the angle and frequency relations than streams that fell in more recently.
Fig. 13 Hessians H_{ij}, timeaveraged Hessians Q_{ij} (both in units of 10^{3} kpc^{2}), and their ratios h_{i} and q_{i} for orbit O7. Left panel: the dashdotted lines show H_{ij} in the static potential, the solid lines the H_{ij} in the timedependent potential, and the dashed lines Q_{ij} in the timedependent potential. We note that  H_{r}r  >  H_{rφ}  >  H_{φφ} , and similarly for Q_{ij}. The middle panel shows that h_{φ}>q_{φ} at all times and that both increase with time. On the other hand, h_{r}<q_{r} at all t, and both decrease with time. Right panel: the ranking of the h_{i} for the different orbits. Both h_{φ} and h_{r} are ranked by the ratio Ω_{φ}/ Ω_{r}, indicating the dependence on the type of orbit. The q_{i} are ranked in the same way. 

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In Fig. 14 we show the predictions of the slope differences for the angle and frequency spaces for the orbits in Table 1. With increasing amount of time evolution by changing the growth parameter a_{g}, the difference in slope also becomes larger. Another interesting prediction is that the more circular orbits have a larger slope difference, although this is at a small level. We gauge the magnitude of the anglefrequency misalignment by using the aperture angle Ψ_{Δθ, ΔΩ} between the fitted lines in the angle and frequency space (as also used by Sanders & Binney 2013b,a) (34)where S(i) = tan(Ψ_{i}), and we have used that the difference in slopes is small^{7}. With this definition of the anglefrequency misalignment, typical values of Ψ_{Δθ, ΔΩ} are around 1.5° for a_{g} = 0.8.
It has been discussed earlier that a stream does not exactly follow an orbit, and the small difference between these two trajectories is known as the streamorbit misalignment. The characteristic magnitude of this can be found from (35)where S(θ_{cm}) = tanΨ_{θcm} is the slope of the straight line traced by the centre of the mass of the progenitor in angle space for a static potential (see also Fig. 12). The typical order of magnitude of Ψ_{S, O} for the Carina progenitor is about 1 degree, similar to what was found in Sanders & Binney (2013b) for a static logarithmic axisymmetric potential, and also similar to values of the streamorbit misalignment in the isochrone potential of Eyre & Binney (2011). We note that the anglefrequency differences in slope that we find are of the same order of magnitude as the streamorbit misalignment.
Fig. 14 Slope differences between the streams in angle and in frequency space as a function of growth parameter a_{g}, as predicted by our analytic model using Eqs. (23) and (26) for our experiments. 

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When comparing simulations with and without time evolution, the streamorbit misalignment can also be used as an indicator of time evolution. In Fig. 6 we saw that the angular position of the stream and progenitor orbit petals one radial period away from the current progenitor location are different for the timedependent case. This angular separation can be derived as follows. For the progenitor, the location of the petal is simply the precession of the orbit in one radial period, that is, ψ_{cm} = 2πS(θ_{cm}) = 2πΩ_{φ}/ Ω_{r}. For the stream, this difference in radial angle from the progenitor is ΔΘ_{r} = 2π, and therefore the angle of the petal of the stream is ψ_{stream} = 2πS(Δθ). Therefore the streamorbit misalignment in azimuthal angle is (36)Increasingly higher growth rates of the potential will yield also larger angular streamorbit separations because S(Δθ) changes by the amount in Fig. 14 (S(ΔΩ) and S(θ_{cm}) are by construction the same at the final time). By multiplying this by 360° to find the difference at the first petals next to the progenitor, we find that these differences can reach up to 10 degrees in our experiments.
In summary, stream particles are distributed following straight lines in angle space when computed using the correct potential and otherwise show a wiggly behaviour and a broken energy gradient. These straight lines have the same slope in frequency space in the static case. If the potential has evolved in time, then the slope in frequency space is typically shallower than in angle space, to an extent that depends on the growth of the gravitational potential.
4.2.3. Validation of the analytic model
We expect our analytic model to faithfully reproduce the behaviour of the testparticle simulations except in some cases. We neglected two effects that can modify these slopes in the derivations above. The first appears when the initial angle spread of the progenitor is comparable to its current extent, in which case the former needs to be taken into account. Since the initial extent typically is unknown, it is better to use very extended streams to derive the evolution in time of the host potential. The second effect is when the time evolution of the potential is nonadiabatic. In this case, the higher order terms of Eq. (13) have to be taken into account.
To confirm this, we used three simulations with different growth factors a_{g} = {0.0,0.4,0.8}, but with the same initial action distribution as in the a_{g} = 0.8 case by using the transformation described in Eq. (10).
Fig. 15 Examples of the slope differences between the angle and frequency distributions (top panels) and histograms of the spread of Δθ_{r}(0)/Δθ_{r}(t_{f}) (bottom panels). In the top panels, the blue crosses indicate values from the full simulation, while the green lines are the predictions from our analytic model. The red crosses are the slopes measured when the initial spreads from the simulations are removed. All orbits now align with the model when a_{g} = 0. For large a_{g} the more circular orbits such as orbit O15 deviate strongly from the model because of nonadiabaticity. 

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Fig. 16 Angle and frequency space plots and residuals of the frequency space fits of all 15 streams for 1% distance (and proper motion) errors in the timedependent potential. The streams are centred on the position of the centre of mass of the progenitor in the errorfree case. The black points are errorconvolved, while those in yellow are errorfree and only shown in the bottom row. The residuals were computed by subtracting the bestfit straight line to the errorfree frequency distribution (green line) from ΔΩ_{φ}. The text in the panels shows the relative difference in the slopes for the errorconvolved and errorfree cases derived in angle space E_{θ} and in frequency space E_{Ω} (i.e. using the red vs. green straight lines, respectively). The panels for which E_{i}< 0.005 are marked with a green box. The difference in slope in angle space clearly is generally far below this value, while the frequencies are much more strongly affected by the errors. 

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Figure 15 shows the difference between the slopes in angle and in frequency spaces for our analytic model. In this figure, the green line shows the prediction of our model using Eqs. (25) and (27), and the actual measured slope differences from the testparticle simulations are shown as blue crosses. This comparison shows that the agreement is excellent, as exemplified for Orbit O7 in the left panel, and this is true for most of the orbits we explored. However, there are a few cases, such as those shown in the panels on the right, where the model fails.
Fig. 17 Selection of the seven best orbits of Fig. 16, but now with 10% parallax (and proper motion) errors. The colours, lines, and insets are the same as in Fig. 16. With these 10× larger distance errors, the angle slopes of the streams are still well measured for most orbits, while the frequency slopes generally are not. 

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Fig. 18 Selection of the orbits of Fig. 16 with 10% parallax errors, but now with two cuts: σ_{d} ≤ 2 kpc and  Ω_{r}−⟨Ω_{r}⟩  ≤ SD_{Ωr}. The colours are the same as in Fig. 17, with the addition that green points represent the particles that remain after the cuts. The grey vertical dashed lines indicate ⟨Ω_{r}⟩ and ⟨Ω_{r}⟩ ± SD_{Ωr} applied after the distance cut. The insets in the top panels show the number of remaining particles after the cuts N_{cut}, while those in the bottom panels are the number of particles within a distance of 20 kpc from the Sun N (d< 20 kpc). 

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For these two cases, the initial extent of the progenitor in angle space cannot be neglected, as can be seen from the bottom panels. This can either be because the streams are relatively short or because the initial spread in angles is large. When the initial angle spreads as given by Eqs. (8) and (26) are removed, the simulations match the model significantly better, as indicated by the red crosses.
The rightmost panel still shows some disagreement, especially for higher values of the growth factor a_{g}. This behaviour stems from the nonadiabatic evolution of the orbit, so that higher terms in Eq. (12), and the last approximation in Eq. (26), fail. An indication that these orbits evolved nonadiabatically is for example that J_{r}(0) /J_{r}(t_{f})−1 ≈ 0.18 for orbit O15. The orbits that are more circular typically suffer more strongly from this effect. This implies that radial orbits may be preferred to obtain the amount of time evolution for a stream that evolved in a smoothly growing potential such as ours.
5. Observational prospects
Now that we have determined the signature of time evolution of a gravitational potential through the difference in slopes in the angle and frequency spaces, we are interested in establishing whether this effect is measurable. This is particularly relevant in the context of the upcoming catalogues from the Gaia satellite.
We therefore convolved our simulated data in observable space with errors. The largest uncertainties typically come from the errors in distance and proper motion. We investigated two cases for the errors in the parallax: 1% (σ_{π}/π = 0.01) and 10% (σ_{π}/π = 0.1), while the proper motion errors are set to be σ_{μ} = 0.5σ_{π}), as given by the Gaia mission error estimates. We assumed radial velocity errors of 1 km s^{1}, which is the level obtainable from followup surveys of the Gaia satellite such as 4MOST (de Jong et al. 2012) and WEAVE (Dalton et al. 2012). Although this error may be seen as small, we have found no significant dependence on the radial velocity error, even if this was as large as 10 km s^{1}. After applying error convolution, we converted the data back to Cartesian coordinates.
In Fig. 16 we show the structure in angle (top row) and in frequency (middle row) space for the 1% distance errors for all 15 orbits evolved in the timedependent potential. The bottom row panels show the residuals in frequency space after subtracting the fitted slope from the errorfree case (green line). Here the black points correspond to the errorconvolved case, while the yellow points are error free.
We define the relative difference in slope in the frequency E_{Ω} and angle E_{θ} spaces after error convolution as with the representing the slopes derived by fitting the distributions with errors. The various panels in Fig. 16 show that this relative difference typically varies from 10^{5} up to 6 × 10^{4} for E_{θ} and between 3 × 10^{4} up to 10^{2} for E_{Ω}, indicating that errors affect the distribution of frequencies more severely than that of angles.
An estimate of tolerable errors may be derived from the following arguments. If ΔS is the slope difference between frequency and angle space (typically a few %), then we can tolerate (39)The panels that satisfy this requirement are highlighted with a green box. The very radial orbits that have small pericentres are mostly selected in this way. These streams have many stars relatively near the Sun (which is positioned at 8 kpc from the Galactic centre along the x axis). The more radial streams also have a much broader spread in J_{r}, which is slightly less affected by the errors than the more circular orbits, which have a broader spread in angular momentum. We conclude that the 1% distance errors allow us to uncover the time evolution for at least half of our orbits when the growth factor is a_{g} = 0.8. However, if we were to consider a growth factor a_{g} = 0.4, the misalignment between angle and frequency space would typically be reduced by a factor 2, and the errors would considerably hinder measuring the time evolution for more slowly evolving potentials.
In Fig. 17 we show the seven best orbits from Fig. 16, but now with 10% distance errors. The colours and insets are the same as in Fig. 16. As the insets and green boxes show, the angles are still quite well measured, but the frequency slope is not. Only one very radial orbit (that comes close to the Sun) presents an acceptable level of uncertainty. There is significant structure in the bottom panels, which depict the residuals between the distribution in frequency space before and after error convolution. For each experiment this is a result of superposing individual wraps with varying distance gradients, and this, after a distancedependent error convolution, causes different frequency distributions. The bowtielike structure is thus the result of the overlap of multiple wraps that are differently distorted in frequency space. The more circular orbits O15 and O9 only show one leg of these bowtielike structures because basically just slightly more than one wrap is present for these experiments.
Given that the 10% errors make it challenging to fit a slope in frequency space, but less so in angle space, we investigated methods for cutting the data and retaining the highest quality measurements. Figure 18 shows the result of combining a distance cut and a frequency cut for the same seven orbits as in Fig. 17. The cuts are given by (40)
with ⟨Ω_{r}⟩ the mean frequency from the data and SD_{Ωr} the standard deviation of Ω_{r}, both computed after the distance cut. The distance error cut improves both the tangential velocities and the distances, and its effect is to mainly select particles at pericentre, as seen in the top panels of this figure. Our cut at 2 kpc essentially removes particles with errors larger than 10% at 20 kpc. The motivation for imposing a frequency cut is to remove outliers. The vertical dashed lines in the frequency space of Fig. 18 show the mean and standard deviation of ΔΩ_{r} with errors, and they encompass the errorfree ΔΩ_{r} distribution indicated in yellow quite well. The combination of these cuts still leaves many particles in the stream, as indicated by the insets in the figure, except for orbits O15 and O9, which basically have no or too few particles closer than 20 kpc, and hence have distance errors larger than 2 kpc. In conclusion, a cut in frequency and distance leads to satisfactory improvements, except when there are too few particles and for a few pathological cases. Such a cut might therefore be used to measure the slope in frequency space, but is not necessary in angle space.
6. Discussion and conclusions
We have investigated the effect of an adiabatically growing timedependent potential on streams. To this end we used the insideout growing spherical NFW potential from Buist & Helmi (2014) as a background for modelling the evolution of a set of 15 testparticle streams.
We performed a series of numerical experiments starting from different initial conditions that were mostly ran in a quite strongly growing model in which the enclosed mass within the orbits that we explored approximately doubled. These experiments showed that the precession rate of streams, that is, the angular location of the “apocentres” of streams in the orbital plane, is significantly different when the potential has evolved in time. Time evolution typically leads to a misalignment or angular difference of ~10° in comparison to the static case, and this is roughly independent of the progenitor size. To be able to detect this effect, however, streams need to be sufficiently long, meaning that they need to have wrapped around more than once.
We then analysed the behaviour of streams in actionangle coordinates. Streams typically appear as extended linear structures in angle and frequency space, also in the timedependent case. We found that time evolution causes these distributions to differ in slope, unlike what is expected for a static potential. To explain these findings, we developed an analytic description of a stream in an adiabatically changing timedependent potential. This allowed us to predict that the difference in slopes in angle and in frequency space is of order ~0.005–0.025, that is, 0.3°–1.5°, for potentials with a growth factor ranging from 0.2 to 0.8. Experiments for which the time evolution signal is most reliably recovered were those that initially had a small size and evolved in an adiabatic way. This condition is most easily satisfied for the more radial orbits.
Although the predicted effect is small, we explored whether it would be observable with the nextgeneration facilities for mapping the Galaxy, such as the Gaia satellite mission (Prusti 2012) and the followup surveys 4MOST (de Jong et al. 2012) and WEAVE (Dalton et al. 2012). When assuming an error in parallax of 1% (and half of that in the proper motion), we found that for about half of the streams the timedependence signature is expected to be measurable. When the errors in parallax (and consequently in proper motion) are increased to 10%, only 1 of our 15 streams can be used to determine the time evolution. Reasonable additional cuts in distance errors and in frequency space (because this is most strongly affected by errors), allowed the time evolution to be determined for an additional four streams. The best results were obtained for streams that are very radial and have small pericentres (inside the solar circle). This is predominantly because these streams have many stars close to the Sun and therefore have smaller observational uncertainties. There is no guarantee that streams with such characteristics will be present in the Gaia dataset, of course, both because of the requirement on their orbital properties and on the rather optimistic assumptions on the distance and proper motion errors.
Another important issue is that the correct potential is necessary to derive the correct angle and frequency space distributions. Fortunately, an incorrect potential distorts the distribution in angle and in frequency spaces in such a manner that each space can be used independently to improve the estimation of the potential for sufficiently long streams. For short streams (e.g. with only one wrap), the misalignment observed might be confused with time evolution instead of the incorrect assumptions about the potential. The use of short streams might therefore induce a bias in the derived values of the characteristic parameters of the potential or its time dependence.
By construction, we neglected the effect of selfgravity in our experiments. Selfgravity would create a gap in the action space between (the progenitor and) the leading and trailing streams (Gibbons et al. 2014), because the particles released at specific points along the orbit (rather than continuously) are offset in energy (Johnston 1998). This structure will most likely also be apparent in the angle and frequency distributions of the particles that make up the stream (Eyre & Binney 2011). Moreover, when close to the progenitor, released particles still experience a gravitational pull by the progenitor (Choi et al. 2009), and epicyclic oscillations are seen in streams in Nbody simulations (Küpper et al. 2010, 2012). These effects may complicate fitting a straight line to the distribution and determining its slope accurately, but after the particles become unbound, the dynamics is essentially the same as in our testparticle integrations (Sanders & Binney 2013b).
Other interesting timedependent effects may be involved in shaping streams and complicate interpretations. Interactions with dark subhaloes orbiting the Galactic halo will affect the structure of streams and create gaps, for example (Yoon et al. 2011; Carlberg 2013; Ngan & Carlberg 2014). Dwarf galaxies as massive as the Large and Small Magellanic Clouds are able to significantly perturb the potential (VeraCiro & Helmi 2013), and might induce nonadiabatic changes in the stream orbits (Gómez et al. 2015). It therefore seems important to try and understand these less secular effects on the dynamical evolution of streams.
We have presented here the first steps towards understanding the imprints of time evolution. More explorations are necessary because we did not study other density profiles or deviations from spherical symmetry, nor did we take into account the effects of a live halo or a (growing) disk. It may be possible to extend our method to any potential for which actionangle coordinates can be derived or approximated, and we do expect the general behaviour to be similar when the potential is growing adiabatically. Overall, we expect the imprint of the smooth mass growth of the Galactic dark halo to be present in streams and to a have a small but nonnegligible magnitude.
We recall that the ratio of angular to radial frequencies for any gravitational potential is limited by the homogeneous sphere case, for which Ω_{φ}/ Ω_{r} = 1/2 and the Kepler case, for which Ω_{φ}/ Ω_{r} = 1. As mass increases and the orbit shrinks, we may say, effectively, that the stream moves farther away from experiencing a Kepler potential (and hence a steeper slope) and closer to the homogeneous sphere (a shallower slope, as also seen in Gómez & Helmi 2010), although the NFW potential is neither of these limiting cases.
Acknowledgments
H.J.T.B. and A.H. gratefully acknowledge financial support from ERCStarting Grant GALACTICA240271. We thank the anonymous referee for a constructive report that helped improve this manuscript. H.J.T.B. thanks Robyn E. Sanderson for the many interesting and useful discussions.
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Online material
Appendix A: Computing the angles
The angles result from the derivatives of the generating function W(x,J) w.r.t. the actions (A.1)(Binney & Tremaine 2008, Eq. (3.204)). The complete generating function for a spherical system is given by (modified from Eq. (3.220), Binney & Tremaine 2008) (A.2)where we integrate over the particles trajectory in phase space, which means for example that during a whole radial period, the particle transverses twice the branch from pericentre to apocentre, but once in reversed direction. The latitudinal momentum p_{ϑ} is (A.3)where cosi = L_{z}/L. The radial momentum p_{r} is (A.4)where L = J_{θ} +  J_{φ}  and J_{φ} ≥ 0 is assumed^{8}.
We find the radial angle as (A.5)where we note that the angles are always defined modulo 2π because there is no information on how many loops a particle made around the Galactic centre. The derivative of the generating function is given by (A.6)where the conditions on p_{r} are necessary to take the right branch of f_{1}. After one full period, we find θ_{r} = 2π as expected.
For the azimuthal angle we find (A.7)where we find φ using the (quadrantaware) arctangent (A.8)The derivative W_{r,H} has already been worked out for θ_{r}, and the other derivatives are
The function W_{ϑ,Jφ} is oscillatory in nature (w.r.t. ϑ), while the combination W_{r,Jφ} + Ω_{φ}W_{r,H} is also oscillatory (w.r.t. r): after one radial period it evaluates to −2Lf_{2}(r_{apo}) + 2Ω_{φ}f_{1}(r_{apo}) = 0.
The latitudinal angle is given by (A.11)Because we assume J_{φ} ≥ 0, we find W_{r,Jϑ} = W_{r,Jφ} and Ω_{ϑ} = Ω_{φ}. The remaining derivative of the generating function is (A.12)where the term W_{r,Jϑ} + Ω_{ϑ}W_{r,H} vanishes after one radial period, while the term W_{ϑ,Jϑ} contains the dependence on ϑ and increases by 2π after one period in ϑ.
Appendix B: Transformation equations
The linearised transformation between actionangle coordinates and Cartesian coordinates is (B.1)For simplicity, we provide here the matrix for the 2D case (i.e. when the orbit is in the plane). In that case, J_{θ} = 0 and J_{φ} = L = L_{z}, so that we find (B.2)where the above terms are given by (B.7)The functions κ and η are and the W_{Ji,Jj} are found by differentiating the generating function
All Tables
All Figures
Fig. 1 Increase of the enclosed mass for several orbits for our timedependent potential with a growth factor of a_{g} = 0.8. The dashed lines show the enclosed mass within the final value of their apocentre. Since the apocentric distances shrink with time, we show the mass enclosed within the timedependent apocentre values with solid lines. The integration time span for the streams is t ~ 7–8 Gyr, and the enclosed mass approximately doubles over this timescale. 

Open with DEXTER  
In the text 
Fig. 2 Relation between the coordinates and the angles in the plane of the orbit. The top panel shows that the radial angle θ_{r} increases by 2π in one radial oscillation. In the bottom panel we have plotted φ (red) and θ_{φ} (blue) as functions of θ_{r}. After one radial period, both angles reach the same value 2πΩ_{φ}/ Ω_{r}. 

Open with DEXTER  
In the text 
Fig. 3 Distribution in action (left), frequency (second panel) and angle space (right) for particles in a stream, and centred on the centre of mass of the progenitor system. The colours represent the energy gradient, where red is for the trailing and green for the leading arms. 

Open with DEXTER  
In the text 
Fig. 4 Streams from three progenitor sizes for each of the 15 orbits evolved in the timedependent a_{g} = 0.8 potential. The left, middle, and right panels correspond to the “Carina”, “Sculptor”, and “Sagittarius”like progenitors, respectively (see Table 2 for their properties). Particles in green are more bound to the host galaxy (leading arm), while those in red are less bound (trailing arm) than the progenitor. The dashed curves are the progenitor orbits evolved in today’s potential, with the green integrated forward in time for the leading arm and red backwards for the trailing arm. The current position of the progenitor is indicated with a red cross. 

Open with DEXTER  
In the text 
Fig. 5 Radial vs. angular distribution of particles in the orbital plane for experiment O7 for the different progenitors in the timedependent case. The dashed curves show the orbit of the centre of mass of the system integrated long enough to roughly reproduce the lengths of the streams. The variations in the apocentric distances are a reflection both of time evolution and of the energy gradient present along a stream. The difference in angular location of the apocentre, on the other hand, is a clear imprint of time evolution, as can be seen by comparing to e.g. Fig. 7. 

Open with DEXTER  
In the text 
Fig. 6 Streams from the Carina progenitor in the evolving and in the nonevolving potential. The streams in the left and centre have the same initial distribution in configuration and velocity space. Those in the right panels have the same initial actionangle distribution as the timeevolving potential (middle panel), but are evolved in a static potential. The colour coding is the same as in the previous figure. The streamorbit misalignment can be seen by looking at the azimuthal angle of the petals starting from one radial period away from the progenitor, whose position is indicated with a red cross. 

Open with DEXTER  
In the text 
Fig. 7 Radial vs. angular distribution of particles in the orbital plane for experiment O7 for the Carinalike progenitor in the static case (left), timedependent case (middle), and static case with the same initial actionangle distribution as in the middle panel. The dashed curves show the orbit of the centre of mass of the system integrated in the presentday potential for the left and right panels, and in the evolving potential for the middle panel. For the static cases, the variations in the apocentric distances are a reflection of the energy gradient present along the stream, while a second effect is present in the middle panel because of time evolution. In this case, the difference in angular location of the apocentre is also much more pronounced and systematically increases for older wraps. 

Open with DEXTER  
In the text 
Fig. 8 Actionspace distributions for a sample of four streams from Fig. 6, measured with respect to the centre of mass of the progenitor at the final time. The colours of the particles represent the energy gradient, such that green is the leading arm and red the trailing arm. In the static cases, the initial and final distributions coincide exactly, but in the timedependent case there can be small deviations if the orbit is not in the adiabatic regime, as can be seen by comparing the middle and right panels for orbits O11 and O15. The left panels show a smaller spread because the timedependent cases start farther outwards and in an initially much lighter potential. 

Open with DEXTER  
In the text 
Fig. 9 Response of the radial action and the radial frequency to a timedependent potential for orbit O7 (Table 1). For this orbit, the action shows a nonsecular oscillation that decreases in amplitude as the rate of change of the potential decreases. The value of Ω_{r} changes significantly with time, and here there are also oscillations that become smaller as the change rate of the potential decreases. The period of the oscillations corresponds with the radial period. The evolution of J_{r} has been quite adiabatic because it oscillates around a limiting value, which is the starting value when the particles were released at pericentre. 

Open with DEXTER  
In the text 
Fig. 10 Angle space of stream O7 (see Table 1) evolved in a timedependent potential, but where the angles have been computed with different (incorrect) parameters. The central panel shows the correct parameters, while r_{s} is changed vertically and M_{s} horizontally by 10% and 30%. The colour coding indicates the energies, with green representing the leading arm (more bound) and red the trailing arm (less bound). 

Open with DEXTER  
In the text 
Fig. 11 Angle space of streams O11 (top) and stream O1 (bottom) evolved in a timedependent potential, but where the angles have been computed with different (incorrect) parameters. We note that although the distortions in angle space are less pronounced for the more radial orbit O1, the energy gradient (indicated by the colour gradient and coding used before) is not preserved. 

Open with DEXTER  
In the text 
Fig. 12 Lines fitted to the angle space (red dashed line) and the frequency space (blue line) of stream O7 evolved in a timedependent (top) and static potential (bottom) using the same (correct) final potential. Additionally, the green line shows the track of the progenitor assuming the potential is static (i.e. θ_{cm}(t) = Ω_{cm}(t_{f})t), and the grey line shows the line fitted to the frequency space at the beginning of the simulation. The inset labels show the numerical values of the aperture angle (misalignment) between the stream and the (static) progenitor orbit Ψ_{S, O}, and between the stream in angle and in frequency space Ψ_{Δθ, ΔΩ} (see Eqs. (34) and (35)). 

Open with DEXTER  
In the text 
Fig. 13 Hessians H_{ij}, timeaveraged Hessians Q_{ij} (both in units of 10^{3} kpc^{2}), and their ratios h_{i} and q_{i} for orbit O7. Left panel: the dashdotted lines show H_{ij} in the static potential, the solid lines the H_{ij} in the timedependent potential, and the dashed lines Q_{ij} in the timedependent potential. We note that  H_{r}r  >  H_{rφ}  >  H_{φφ} , and similarly for Q_{ij}. The middle panel shows that h_{φ}>q_{φ} at all times and that both increase with time. On the other hand, h_{r}<q_{r} at all t, and both decrease with time. Right panel: the ranking of the h_{i} for the different orbits. Both h_{φ} and h_{r} are ranked by the ratio Ω_{φ}/ Ω_{r}, indicating the dependence on the type of orbit. The q_{i} are ranked in the same way. 

Open with DEXTER  
In the text 
Fig. 14 Slope differences between the streams in angle and in frequency space as a function of growth parameter a_{g}, as predicted by our analytic model using Eqs. (23) and (26) for our experiments. 

Open with DEXTER  
In the text 
Fig. 15 Examples of the slope differences between the angle and frequency distributions (top panels) and histograms of the spread of Δθ_{r}(0)/Δθ_{r}(t_{f}) (bottom panels). In the top panels, the blue crosses indicate values from the full simulation, while the green lines are the predictions from our analytic model. The red crosses are the slopes measured when the initial spreads from the simulations are removed. All orbits now align with the model when a_{g} = 0. For large a_{g} the more circular orbits such as orbit O15 deviate strongly from the model because of nonadiabaticity. 

Open with DEXTER  
In the text 
Fig. 16 Angle and frequency space plots and residuals of the frequency space fits of all 15 streams for 1% distance (and proper motion) errors in the timedependent potential. The streams are centred on the position of the centre of mass of the progenitor in the errorfree case. The black points are errorconvolved, while those in yellow are errorfree and only shown in the bottom row. The residuals were computed by subtracting the bestfit straight line to the errorfree frequency distribution (green line) from ΔΩ_{φ}. The text in the panels shows the relative difference in the slopes for the errorconvolved and errorfree cases derived in angle space E_{θ} and in frequency space E_{Ω} (i.e. using the red vs. green straight lines, respectively). The panels for which E_{i}< 0.005 are marked with a green box. The difference in slope in angle space clearly is generally far below this value, while the frequencies are much more strongly affected by the errors. 

Open with DEXTER  
In the text 
Fig. 17 Selection of the seven best orbits of Fig. 16, but now with 10% parallax (and proper motion) errors. The colours, lines, and insets are the same as in Fig. 16. With these 10× larger distance errors, the angle slopes of the streams are still well measured for most orbits, while the frequency slopes generally are not. 

Open with DEXTER  
In the text 
Fig. 18 Selection of the orbits of Fig. 16 with 10% parallax errors, but now with two cuts: σ_{d} ≤ 2 kpc and  Ω_{r}−⟨Ω_{r}⟩  ≤ SD_{Ωr}. The colours are the same as in Fig. 17, with the addition that green points represent the particles that remain after the cuts. The grey vertical dashed lines indicate ⟨Ω_{r}⟩ and ⟨Ω_{r}⟩ ± SD_{Ωr} applied after the distance cut. The insets in the top panels show the number of remaining particles after the cuts N_{cut}, while those in the bottom panels are the number of particles within a distance of 20 kpc from the Sun N (d< 20 kpc). 

Open with DEXTER  
In the text 
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