[yt-users] Error in streamline plotting

29 Jan 2018

      Dear yt:

I am getting the following error for the script (see below). Could you let
me know what is causing  it? Thank you in advance

Error:
yt.utilities.exceptions.YTUnitOperationError: The addition operator for
YTArrays with units (km) and (1) is not well defined.

Script:
import yt
import numpy as np
import matplotlib.pylab as pl
import matplotlib.pyplot as plt
import matplotlib.colors as colors
from matplotlib.colors import LogNorm

from yt.visualization.api import Streamlines
from yt.units import km
from mpl_toolkits.mplot3d import Axes3D

ms = 24000000
vector_max=ms-(ms/3)
ms1=ms-vector_max
dims = (200,200,200)

x =
np.genfromtxt("/work/jbi157/MODEL7/UPDATE_B/yo_n_t0.mtx",skip_header=2,usecols=1,
dtype="f8")
x = x.reshape((8000000, 3), order="F")

field1 = x[:,2].reshape(dims, order="F")
field2 = x[:,1].reshape(dims, order="F")
field3 = x[:,0].reshape(dims, order="F")

data = dict(cutting_plane_velocity_x = field1,
            cutting_plane_velocity_y = field2,
            cutting_plane_velocity_z = field3)

bbox = np.array([[-100, 99], [-100, 99], [-100, 99]])

pf = yt.load_uniform_grid(data, dims, km, bbox=bbox, nprocs=1)

L = [0,1,0] # vector normal to cutting plane
north_vector = [0,1,1]

slc = yt.OffAxisSlicePlot(pf, L, 'cutting_plane_velocity_x',
center=[0,0,0], width=(180,'km'), north_vector=north_vector)

vel = slc._frb['cutting_plane_velocity_z']
U = slc._frb['cutting_plane_velocity_x']
V = slc._frb['cutting_plane_velocity_y']

extentx = [slc.xlim[i].in_units('km') for i in (0, 1)]
extenty = [slc.ylim[i].in_units('km') for i in (0, 1)]
extent = extentx + extenty

x = np.linspace(extentx[0], extentx[1], vel.shape[0])
y = np.linspace(extenty[1], extenty[0], vel.shape[1])

X, Y = np.meshgrid(x, y)

normalize = True
if normalize is True:
        N = np.sqrt(U**2+V**2)
        U /= N
        V /= N

norm = colors.Normalize(vmin=vel.min(), vmax=vel.max())
factor = 1
#plt.quiver(X[::factor, ::factor], Y[::factor, ::factor], U[::factor,
::factor], V[::factor, ::factor])

plt.streamplot(X,Y,U,V,norm='True')

#plt.imshow(vel.d, extent=extent)
plt.colorbar()
plt.xlabel("x")
plt.axis([-100, 99, -100, 99])
plt.savefig('L(1,0,0) N(0,1,1)')
#slc.save()

On Mon, Jan 29, 2018 at 2:52 PM,  wrote:
...
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Today's Topics:
1. CLARIFICATION ON FIELD TYPES (Vadlamani Samhitha)
   2. Re: CLARIFICATION ON FIELD TYPES (Nathan Goldbaum)
   3. Re: CLARIFICATION ON FIELD TYPES (Vadlamani Samhitha)
   4. Re: ROTATION CURVE PLOTS IN YT (Vadlamani Samhitha)
----------------------------------------------------------------------
Date: Mon, 29 Jan 2018 19:39:25 +0100
From: Vadlamani Samhitha 
Subject: [yt-users] CLARIFICATION ON FIELD TYPES
To: Discussion of the yt analysis package 
Message-ID:

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Hi yt-users,
I am a newbie in using YT. I read through the documentation of field types
but I still have some confusion in understanding when to use different
field types, as in:
(1) 'io' vs 'all' (from what I understand, both are used for particles but
I don't get the minute difference)
(2) 'ramses' vs 'index' vs 'gas' (fluids described on the grid, I suppose?)
It would be really helpful if someone could provide an elaborate
explanation on these.
--001a113a8b64cce13c0563ee9005
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Hi yt-users,=C2=A0<div><br></div><div>I am a newbie in
usi=
ng YT. I read through the documentation of field types but I still have
som=
e confusion=C2=A0in understanding when to use different field types, as
in:=
=C2=A0</div><div><br></div><div>(1) 'io' vs 'all' (from
wha=
t I understand, both are used for particles but I don't get the minute
=
difference)</div><div>(2) 'ramses' vs 'index' vs
'gas&#=
39; (fluids described on the grid, I suppose?)</div><div><br></div><div>It
=
would be really helpful if someone could provide an elaborate explanation
o=
n these.=C2=A0 =C2=A0=C2=A0</div></div>
--001a113a8b64cce13c0563ee9005--
------------------------------
Date: Mon, 29 Jan 2018 12:47:09 -0600
From: Nathan Goldbaum 
Subject: [yt-users] Re: CLARIFICATION ON FIELD TYPES
To: Discussion of the yt analysis package 
Message-ID:

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On Mon, Jan 29, 2018 at 12:39 PM, Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
...
Hi yt-users,
I am a newbie in using YT. I read through the documentation of field
types
but I still have some confusion in understanding when to use different
field types, as in:
(1) 'io' vs 'all' (from what I understand, both are used for particles
but
I don't get the minute difference)
This distinction only matters if there are multiple types of particles in a
single simulation. For example, Gadget data has 5 different particle types
on disk, 'halo', 'disk', 'stars', 'bulge', and 'gas'. If I load a Gadget
dataset with yt I can access the particles in each of these particle types
separately by prefixing the particle field I want to access with the
particle type I want to access.
"all" is a particle union (see
http://yt-project.org/docs/dev/analyzing/filtering.html#particle-unions)
that corresponds to the union between all on-disk particle types. If you
access an "all" field, you will get back the field values for the union of
all of the particles in the simulation. Only fields that are defined for
all particle types are defined for the "all" particle union.
Since ramses only has one particle type, we call that type "io". For RAMSES
(and Enzo and several other formats where all the particles are mixed
together on disk) "io" and "all" are interchangeable.
...
(2) 'ramses' vs 'index' vs 'gas' (fluids described on the grid, I
suppose?)
The "ramses" field type corresponds to the on-disk fields in the ramses
outputs. Each of these fields has a corresponding "gas" field that it is
aliased to. For example, ('gas', 'density') is an alias to ("ramses",
"Density").
When you access a "gas" field, by default it will be returned in CGS units.
When you access a "ramses" field, by default it will be returned in code
units.
The 'index' fields are fields that depend on the AMR structure or the
geometry of the data but not the on-disk fields. For example, ('index',
'x'), ('index', 'grid_level'), etc.
Hope that helps,
Nathan
...
It would be really helpful if someone could provide an elaborate
explanation on these.
_______________________________________________
yt-users mailing list -- yt-users@python.org
To unsubscribe send an email to yt-users-leave@python.org
--94eb2c197fcaa201900563eead13
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...
</div><div><br></div><div>Nathan<br></div><div>=C2=A0</div>
<div><br></div><div>It
=
would be really helpful if someone could provide an elaborate explanation
o=
n these.=C2=A0 =C2=A0=C2=A0</div></div>
<br>______________________________<wbr>_________________<br>
yt-users mailing list -- yt-users@py=
<br><br>On Mon, Jan 29, 2018 at 12:39 PM, Vadlamani Samhitha =
<vadla=
mani.samhitha@gmail.com</a>></span> wrote:<br>Hi yt-users,=C2=A0<div><br></div>
<=
div>I am a newbie in using YT. I read through the documentation of field
ty=
pes but I still have some confusion=C2=A0in understanding when to use
diffe=
rent field types, as in:=C2=A0</div><div><br></div><div>(1) 'io'
vs=
 'all' (from what I understand, both are used for particles but I
d=
on't get the minute difference)</div></div><div><br></div>=
<div>This distinction only matters if there are multiple types of
particles=
 in a single simulation. For example, Gadget data has 5 different particle
=
types on disk, 'halo', 'disk', 'stars',
'bulge&=
#39;, and 'gas'. If I load a Gadget dataset with yt I can access
th=
e particles in each of these particle types separately by prefixing the
par=
ticle field I want to access with the particle type I want to
access.<br><div><br></div><div>"all" is a particle union (see http://yt-project.org/docs/dev/analyzing/filtering.html#particle-unions
">h=
ttp://yt-project.org/docs/dev/analyzing/filtering.html#particle-unions
</a>)=
 that corresponds to the union between all on-disk particle types. If you
a=
ccess an "all" field, you will get back the field values for the
=
union of all of the particles in the simulation. Only fields that are
defin=
ed for all particle types are defined for the "all" particle
unio=
n.<br></div><div><br></div><div>Since ramses only has one particle type,
we=
 call that type "io". For RAMSES (and Enzo and several other
form=
ats where all the particles are mixed together on disk) "io" and
=
"all" are interchangeable.<br></div><div>=C2=A0</div><div>(2)
'ramses=
' vs 'index' vs 'gas' (fluids described on the grid, I
=
suppose?)</div></div></blockquote><div><br></div><div>The
"ramses"=
; field type corresponds to the on-disk fields in the ramses outputs. Each
=
of these fields has a corresponding "gas" field that it is
aliase=
d to. For example, ('gas', 'density') is an alias to
("=
;ramses", "Density").</div><div><br></div><div>When you
acce=
ss a "gas" field, by default it will be returned in CGS units.
Wh=
en you access a "ramses" field, by default it will be returned
in=
 code units.</div><div><br></div><div>The 'index' fields are
fields=
 that depend on the AMR structure or the geometry of the data but not the
o=
n-disk fields. For example, ('index', 'x'),
('index'=
;, 'grid_level'), etc.</div><div><br></div><div>Hope that
helps,
--94eb2c1c1716c1c66a0563f02a60
Content-Type: text/plain; charset="UTF-8"
Yes! Thank you
On Mon, Jan 29, 2018 at 7:47 PM, Nathan Goldbaum 
wrote:
...
On Mon, Jan 29, 2018 at 12:39 PM, Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
...
Hi yt-users,
I am a newbie in using YT. I read through the documentation of field
types but I still have some confusion in understanding when to use
different field types, as in:
(1) 'io' vs 'all' (from what I understand, both are used for particles
but I don't get the minute difference)
This distinction only matters if there are multiple types of particles in
a single simulation. For example, Gadget data has 5 different particle
types on disk, 'halo', 'disk', 'stars', 'bulge', and 'gas'. If I load a
Gadget dataset with yt I can access the particles in each of these
...
types separately by prefixing the particle field I want to access with
...
particle type I want to access.
"all" is a particle union (see http://yt-project.org/docs/
dev/analyzing/filtering.html#particle-unions) that corresponds to the
union between all on-disk particle types. If you access an "all" field,
you
will get back the field values for the union of all of the particles in
particle
the
the
...
simulation. Only fields that are defined for all particle types are
defined
for the "all" particle union.
Since ramses only has one particle type, we call that type "io". For
RAMSES (and Enzo and several other formats where all the particles are
mixed together on disk) "io" and "all" are interchangeable.
...
(2) 'ramses' vs 'index' vs 'gas' (fluids described on the grid, I
suppose?)
The "ramses" field type corresponds to the on-disk fields in the ramses
outputs. Each of these fields has a corresponding "gas" field that it is
aliased to. For example, ('gas', 'density') is an alias to ("ramses",
"Density").
When you access a "gas" field, by default it will be returned in CGS
units. When you access a "ramses" field, by default it will be returned
in
code units.
The 'index' fields are fields that depend on the AMR structure or the
geometry of the data but not the on-disk fields. For example, ('index',
'x'), ('index', 'grid_level'), etc.
Hope that helps,
Nathan
...
It would be really helpful if someone could provide an elaborate
explanation on these.
_______________________________________________
yt-users mailing list -- yt-users@python.org
To unsubscribe send an email to yt-users-leave@python.org
_______________________________________________
yt-users mailing list -- yt-users@python.org
To unsubscribe send an email to yt-users-leave@python.org
--94eb2c1c1716c1c66a0563f02a60
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Yes! Thank you</div><br>On Mon, Jan 29, 2018 at 7:47 PM, Nathan Goldbaum <=
nathan12343@gmail.com</a>></span> wrote:<br><br><br>On Mon, Jan 29, 2018 at 12:39 PM, Vadlamani
Samhith=
a <vadlamani.samhitha@gmail.com</a>></span>
wrote:<br>Hi yt-users,=
=C2=A0<div><br></div><div>I am a newbie in using YT. I read through the
doc=
umentation of field types but I still have some confusion=C2=A0in
understan=
ding when to use different field types, as in:=C2=A0</div><div><br></div>
(1) 'io' vs 'all' (from what I understand, both are
used=
 for particles but I don't get the minute
difference)</div></div><div><br></div></span><div>This distinction only matters if there
ar=
e multiple types of particles in a single simulation. For example, Gadget
d=
ata has 5 different particle types on disk, 'halo',
'disk',=
 'stars', 'bulge', and 'gas'. If I load a Gadget
da=
taset with yt I can access the particles in each of these particle types
se=
parately by prefixing the particle field I want to access with the
particle=
 type I want to access.<br></div><div><br></div><div>"all" is a
p=
article union (see http://yt-project.org/
docs/dev/analyzing/filt=
ering.html#particle-unions" target=3D"_blank">http://yt-project.org/docs/
dev/analyzing/filtering.html#<wbr>particle-unions</a>) that
corresponds =
to the union between all on-disk particle types. If you access an
"all=
" field, you will get back the field values for the union of all of
th=
e particles in the simulation. Only fields that are defined for all
particl=
e types are defined for the "all" particle
union.<br></div><div><=
br></div><div>Since ramses only has one particle type, we call that type
&q=
uot;io". For RAMSES (and Enzo and several other formats where all the
=
particles are mixed together on disk) "io" and "all"
ar=
e interchangeable.<br></div><div>=C2=A0</div><div>(2)
'ramses&=
#39; vs 'index' vs 'gas' (fluids described on the grid, I
s=
uppose?)</div></div></blockquote><div><br></div></span><div>The
"ramse=
s" field type corresponds to the on-disk fields in the ramses
outputs.=
 Each of these fields has a corresponding "gas" field that it is
=
aliased to. For example, ('gas', 'density') is an alias to
=
("ramses", "Density").</div><div><br></div><div>When
yo=
u access a "gas" field, by default it will be returned in CGS
uni=
ts. When you access a "ramses" field, by default it will be
retur=
ned in code units.</div><div><br></div><div>The 'index' fields
are =
fields that depend on the AMR structure or the geometry of the data but
not=
 the on-disk fields. For example, ('index', 'x'),
('ind=
ex', 'grid_level'), etc.</div><div><br></div><div>Hope that
hel=
ps,<br></div><div><br></div><div>Nathan<br></div><div>=C2=
A0</div>=
<div><br></div><div>It would be really helpful if someone could provide an
=
elaborate explanation on these.=C2=A0 =C2=A0=C2=A0</div></div>
<br></span>______________________________<wbr>_________________<br>
yt-users mailing list -- yt-users@python.org</a><br>
To unsubscribe send an email to yt-users-leave@python.org</a><br>
<br></blockquote></div><br></div></div>
<br>______________________________<wbr>_________________<br>
yt-users mailing list -- yt-users@py=
thon.org</a><br>
To unsubscribe send an email to 
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Hi again,
Thanks for all the responses. As Corentin suggested, I tried a ProfilePlot
for just the particles using phi component of the velocity, but I still
don't get a rotational curve atleast close to what is expected. Also, the
velocity seems unreasonably high (10^4 km/s). Any other possible ideas?
"
*filename=3D"SIM001/output_00030/info_00030.txt"*
*ds=3Dyt.load(filename)*
*sp =3D ds.sphere('c', 100*kpc)*
*plot =3D yt.ProfilePlot(sp, "particle_radius",
["particle_spherical_velocity_phi"], weight_field=3DNone)*
*plot.set_unit("particle_spherical_velocity_phi", "km/s")*
*plot.set_unit("particle_radius", "kpc")*
*plot.save()*
"
[image: Inline image 1]
On Sun, Jan 28, 2018 at 4:59 PM, Eric Gentry  wrote:
...
Remember that v_c generally depends on mass at larger radii too; it's
onl=
y
a few special cases where you only need to know the mass enclosed in a
sphere (e.g. spherical mass distribution, or a Mestel disk).  This is
discussed in Binney & Tremaine's book in section 2.6.1.
Unfortunately I don't know a good, general way for calculating v_c off
th=
e
top of my head.
--
Eric Gentry
PhD Candidate
ISB 159 | ericsgentry.com
Astronomy and Astrophysics
University of California, Santa Cruz
On Sun, Jan 28, 2018 at 3:58 AM, Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
...
Hey again,
I thought of a simpler way to get the rotational curves, basically using
the mass enclosed in a sphere
http://yt-project.org/doc/cookbook/calculating_information.html to
calculate the circular velocity. To be more precise, I do the following:
*filename=3D"output_00010/info_00010.txt" *
*ds=3Dyt.simulation(filename)*
*G=3Dyt.YTArray(4*np.pi**2,'au**3/yr**2/Msun')*
*temp=3Dnp.arange(0.5, 40, 0.1)*
*x=3Dyt.YTArray(temp,'kpc')*
*V_c =3D np.array([])*
*for i in x: *
* sp =3D ds.sphere("c", (i, "kpc"))*
* print(i)*
*# This recipe constructs a sphere and then sums the total mass in
particles and fluids in the sphere*
* baryon_mass, particle_mass =3D sp.quantities.total_quantity([
"cell_mas=
s",
"particle_mass"])*
* M_total=3D(baryon_mass+particle_mass).in_units('Msun')*
* circular=3Dnp.sqrt(G*M_total/i).in_units('km/s')*
* V_c=3Dnp.append(V_c, circular)*
*plt.plot(temp,V_c)*
*plt.show()*
but ended up with a curve attached in the link below. But we expect a
flat rotation curve and not keplerian decrease. Is this a valid
approach=
 to
get the rotation curves in YT?
Thanks!
On Fri, Jan 26, 2018 at 2:22 PM, Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
...
Hey thanks, then, are these derived fields computed automatically and
available to access when the data is loaded or does the user have to
manually compute as in
here <http://yt-project.org/doc/developing/creating_derived_
fields.html=
...
...
?
On Thu, Jan 25, 2018 at 6:06 PM, Contact  wrote:
...
From what I see from your mail, it looks like you're only listing the
field_list. You can get a much more comprehensive list using
'ds.derived_field_list' which include e.g. the angular velocity. These
fields aren't directly read from your output but are computed (or
deri=
ved)
quantities, such as the entropy, the dynamical time, =E2=80=A6 and
you=
 an use them
for 1D profiles too.
Corentin Cadiou
On 25 janv. 2018, at 16:16, Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
Sorry, I didn't get what you meant.
On Thu, Jan 25, 2018 at 4:04 PM, Nathan Goldbaum <
nathan12343@gmail.co=
m
...
wrote:
...
You=E2=80=99re looking for the =E2=80=9Cparticle_radius=E2=80=9D
fiel=
d.
On Thu, Jan 25, 2018 at 9:01 AM Vadlamani Samhitha <
vadlamani.samhitha@gmail.com> wrote:
> I see, How about obtaining the rotational curves for gas and matter
> separately and then adding them up? Would that be simpler (even if
i=
ts an
> approximate) instead of considering the potential directly? I
modell=
ed
> stars and dark matter under particles and gas as fluid on the mesh
a=
nd I
> have the following my fields_list: ( I am dealing with cartesian
> coordinates. So, I don't have the spherical coordinates in my
fields=
_list)
>
> *" ('all', 'particle_extra_field_1')*
> *('all', 'particle_extra_field_2')*
> *('all', 'particle_extra_field_3')*
> *('all', 'particle_extra_field_4')*
> *('all', 'particle_extra_field_5')*
> *('all', 'particle_identifier')*
> *('all', 'particle_mass')*
> *('all', 'particle_position_x')*
> *('all', 'particle_position_y')*
> *('all', 'particle_position_z')*
> *('all', 'particle_refinement_level')*
> *('all', 'particle_velocity_x')*
> *('all', 'particle_velocity_y')*
> *('all', 'particle_velocity_z')*
> *('io', 'particle_extra_field_1')*
> *('io', 'particle_extra_field_2')*
> *('io', 'particle_extra_field_3')*
> *('io', 'particle_extra_field_4')*
> *('io', 'particle_extra_field_5')*
> *('io', 'particle_identifier')*
> *('io', 'particle_mass')*
> *('io', 'particle_position_x')*
> *('io', 'particle_position_y')*
> *('io', 'particle_position_z')*
> *('io', 'particle_refinement_level')*
> *('io', 'particle_velocity_x')*
> *('io', 'particle_velocity_y')*
> *('io', 'particle_velocity_z')*
> *('ramses', 'Density')*
> *('ramses', 'Metallicity')*
> *('ramses', 'Pressure')*
> *('ramses', 'var6')*
> *('ramses', 'x-velocity')*
> *('ramses', 'y-velocity')*
> *('ramses', 'z-velocity') "*
>
> So, I am thinking that the highlighted fields in the type 'all'
coul=
d
> be used to compute circular velocity [sqrt(particle_velocity_x^2+
par=
ticle_velocity_y^2)]
> and the radius [sqrt(particle_position_x^2+particle_position_y^2)]
> for particles. And for gas, 'ramses' fields could be used. However,
=
I am
> not sure how to get the radius for the gas in this case. Would this
=
be a
> right approach at all to begin with?
> _______________________________________________
> yt-users mailing list -- yt-users@python.org
> To unsubscribe send an email to yt-users-leave@python.org
>
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_______________________________________________
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_______________________________________________
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_______________________________________________
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</div><div><b><i>plot.save()</i></b></div><div>"</div><div><br></div></div>
<br>On Sun, Jan 28, 2018 at 4:59 PM, Eric Gentry <
Hi again,=C2=A0<div><br></div><div>Thanks for all the
resp=
onses. As Corentin suggested, I tried a ProfilePlot for just the particles
=
using phi component of the velocity, but I still don't get a
rotational=
 curve atleast close to what is expected. Also, the velocity seems
unreason=
ably high (10^4 km/s). Any other possible ideas?=C2=A0</div><div>"<
/di=
v><div><b><i>filename=3D"SIM001/output_00030/info_
00030.txt"</i><=
/b></div><div><b><i>ds=3Dyt.load(filename)</i></b></div><div><b><i>sp =3D
d=
s.sphere('c', 100*kpc)</i></b><br></div><div><b><i>plot =3D
yt.Prof=
ilePlot(sp, "particle_radius", ["particle_spherical_
velocity=
_phi"], weight_field=3DNone)</i></b></div><div><b><i>plot.set_unit(&
qu=
ot;particle_spherical_velocity_phi", "km/s")</i></b><b><i>plot.set_unit("particle_radius",
"kpc")</i>egentry@ucsc.edu
</a>>=
</span> wrote:<br>Remember
=
that v_c generally depends on mass at larger radii too; it's only a
few=
 special cases where you only need to know the mass enclosed in a sphere
(e=
.g. spherical mass distribution, or a Mestel disk).=C2=A0 This is
discussed=
 in Binney & Tremaine's book in section
2.6.1.<div><br></div><div>U=
nfortunately I don't know a good, general way for calculating v_c off
t=
he top of my head.</div></div>
=
<div><div><div><div><br></font></div>-=
-<br>Eric Gentry</font><div>PhD
Candidate<br>
...
<div>ISB 159 | http://ericsgentry.com"
=
target=3D"_blank">ericsgentry.com</a><br></font><div>
color=3D"#888888=
">Astronomy and Astrophysics<br>University of California, Santa
Cruz</font>=
</div></div><div><br></div></div></div></div></div></div></
div></div></div>=
<div><div class=3D"h5">
<br><div class=3D"gmail_quote">On Sun, Jan 28, 2018 at 3:58 AM, Vadlamani
S=
amhitha <span dir=3D"ltr">&lt;<a href=3D"mailto:vadlamani.
samhitha@gmail.co=
m" target=3D"_blank">vadlamani.samhitha@gmail.com</a>&gt;</span>
wrote:<br>=
<blockquote class=3D"gmail_quote" style=3D"margin:0 0 0
.8ex;border-left:1p=
x #ccc solid;padding-left:1ex"><div dir=3D"ltr">Hey again,=C2=A0<div>I
thou=
ght of a simpler way to get the rotational curves, basically using the=C2=
=A0<a href=3D"http://yt-project.org/doc/cookbook/calculating_
information.ht=
ml" target=3D"_blank">mass enclosed in a sphere</a>=C2=A0to calculate the
c=
ircular velocity. To be more precise, I do the
following:</div><div><br></d=
iv><div><div><b><i>filename=3D&quot;output_00010/info_00<
wbr>010.txt&quot;=
=C2=A0</i></b></div><div><b><i>ds=3Dyt.simulation(filename)
</i></b></div><d=
iv><b><i>G=3Dyt.YTArray(4*np.pi**2,&#39;au**3<wbr>/yr**2/
Msun&#39;)</i></b>=
</div><div><b><i>temp=3Dnp.arange(0.5, 40, 0.1)</i></b></div><div><b><i>x=
=3Dyt.YTArray(temp,&#39;kpc&#39;)</i></b></div><div><b><i>V_c =3D
np.array(=
[])</i></b></div><div><b><i>for i in x:=C2=A0</i></b></div><div><b>
<i><span=
 style=3D"white-space:pre-wrap">        </span>sp =3D
ds.sphere(&quot;c&quot;, (i,=
 &quot;kpc&quot;))</i></b></div><div><b><i><span
style=3D"white-space:pre-w=
rap">   </span>print(i)</i></b></div><div><b><i># This recipe constructs
a sp=
here and then sums the total mass in particles and fluids in the
sphere</i>=
</b></div><div><b><i><br></i></b></div><div><b><i><span
style=3D"white-spac=
e:pre-wrap">    </span>baryon_mass, particle_mass =3D
sp.quantities.total_quan=
tity([<wbr>&quot;cell_mass&quot;, &quot;particle_mass&quot;])</
i></b></div>=
<div><b><i><span style=3D"white-space:pre-wrap">
</span>M_total=3D(baryon_m=
ass+particle_<wbr>mass).in_units(&#39;Msun&#39;)</i></b><
/div><div><b><i><s=
pan style=3D"white-space:pre-wrap">     </span>circular=3Dnp.sqrt(G*M_
total/i).=
<wbr>in_units(&#39;km/s&#39;)</i></b></div><div><b><i><span
style=3D"white-=
space:pre-wrap">        </span>V_c=3Dnp.append(V_c,
circular)</i></b></div><div><b=
><i>plt.plot(temp,V_c)</i></b></div><div><b><i>plt.show()</
i></b></div></di=
v><div><br></div><div>but ended up with a curve attached in the link
below.=
 But we expect a flat rotation curve and not keplerian=C2=A0decrease. Is
th=
is a valid approach to get the rotation curves in
YT?</div><div><br></div><=
div>Thanks!</div></div><div class=3D"gmail_extra"><br><div
class=3D"gmail_q=
uote">On Fri, Jan 26, 2018 at 2:22 PM, Vadlamani Samhitha <span
dir=3D"ltr"=
>&lt;<a href=3D"mailto:vadlamani.samhitha@gmail.com"
target=3D"_blank">vadl=
amani.samhitha@gmail.com</a>&gt;</span> wrote:<br><blockquote
class=3D"gmai=
l_quote" style=3D"margin:0 0 0 .8ex;border-left:1px #ccc
solid;padding-left=
:1ex"><div dir=3D"ltr">Hey thanks, then, are these derived fields computed
=
automatically and available to access when the data is loaded or does the
u=
ser have to manually compute as in=C2=A0<div><a href=3D"
http://yt-project.o=
rg/doc/developing/creating_derived_fields.html"
target=3D"_blank">here</a>?=
<br></div></div><div class=3D"m_-2580383644780269033m_-
8722327220951420101H=
OEnZb"><div class=3D"m_-2580383644780269033m_-8722327220951420101h5"><div
c=
lass=3D"gmail_extra"><br><div class=3D"gmail_quote">On Thu, Jan 25, 2018
at=
 6:06 PM, Contact <span dir=3D"ltr">&lt;<a href=3D"mailto:contact@cphyc.me
"=
 target=3D"_blank">contact@cphyc.me</a>&gt;</span> wrote:<br><blockquote
cl=
ass=3D"gmail_quote" style=3D"margin:0 0 0 .8ex;border-left:1px #ccc
solid;p=
adding-left:1ex"><div dir=3D"auto"><div>From what I see from your mail, it
=
looks like you&#39;re only listing the field_list. You can get a much more
=
comprehensive list using &#39;ds.derived_field_list&#39; which include
e.g.=
 the angular velocity. These fields aren&#39;t directly read from your
outp=
ut but are computed (or derived) quantities, such as the entropy, the
dynam=
ical time, =E2=80=A6 and you an use them for 1D profiles
too.</div><div><br=
></div><div>Corentin Cadiou</div><div><div class=3D"m_-
2580383644780269033m=
_-8722327220951420101m_6573092944491014774h5"><div><br>On 25 janv. 2018,
at=
 16:16, Vadlamani Samhitha &lt;<a href=3D"mailto:vadlamani.
samhitha@gmail.c=
om" target=3D"_blank">vadlamani.samhitha@gmail.com</a>&gt;
wrote:<br><br></=
div><blockquote type=3D"cite"><div><div dir=3D"ltr">Sorry, I didn&#39;t
get=
 what you meant.</div><div class=3D"gmail_extra"><br><div
class=3D"gmail_qu=
ote">On Thu, Jan 25, 2018 at 4:04 PM, Nathan Goldbaum <span
dir=3D"ltr">&lt=
;<a href=3D"mailto:nathan12343@gmail.com" target=3D"_blank">nathan12343@
gma=
il.com</a>&gt;</span> wrote:<br><blockquote class=3D"gmail_quote"
style=3D"=
margin:0 0 0 .8ex;border-left:1px #ccc solid;padding-left:1ex"><div><div
di=
r=3D"auto">You=E2=80=99re looking for the =E2=80=9Cparticle_radius=E2=
80=9D=
 field.</div><br><div class=3D"gmail_quote"><div><div
class=3D"m_-258038364=
4780269033m_-8722327220951420101m_6573092944491014774m_-
5999361843722410537=
h5"><div>On Thu, Jan 25, 2018 at 9:01 AM Vadlamani Samhitha &lt;<a
href=3D"=
mailto:vadlamani.samhitha@gmail.com" target=3D"_blank">vadlamani.
samhitha@g=
mail.com</a>&gt; wrote:<br></div></div></div><blockquote
class=3D"gmail_quo=
te" style=3D"margin:0 0 0 .8ex;border-left:1px #ccc
solid;padding-left:1ex"=
><div><div class=3D"m_-2580383644780269033m_-8722327220951420101m_
657309294=
4491014774m_-5999361843722410537h5"><div>I see, How about obtaining the
rot=
ational curves for gas and matter separately and then adding them up?
Would=
 that be simpler (even if its an approximate) instead of considering the
po=
tential directly? I modelled stars and dark matter under particles and gas
=
as fluid on the mesh and I have the following my fields_list: ( I am
dealin=
g with cartesian coordinates. So, I don&#39;t have the spherical
coordinate=
s in my fields_list)<div><br></div><div><i>&quot; (&#39;all&#39;,
&#39;part=
icle_extra_field_1&#39;)</i><div><i>(&#39;all&#39;,
&#39;particle_extra_fie=
ld_2&#39;)</i></div><div><i>(&#39;all&#39;, &#39;particle_extra_field_3&#
39=
;)</i></div><div><i>(&#39;all&#39;, &#39;particle_extra_field_4&#
39;)</i></=
div><div><i>(&#39;all&#39;, &#39;particle_extra_field_5&#
39;)</i></div><div=
><i>(&#39;all&#39;, &#39;particle_identifier&#39;)
</i></div><div><i>(&#39;a=
ll&#39;, &#39;particle_mass&#39;)</i></div><div><i><b>(&#39;all&#39;,
&#39;=
particle_position_x&#39;)</b></i></div><div><i><b>(&#39;all&#39;,
&#39;part=
icle_position_y&#39;)</b></i></div><div><i>(&#39;all&#39;,
&#39;particle_po=
sition_z&#39;)</i></div><div><i>(&#39;all&#39;,
&#39;particle_refinement_le=
vel&#39;)</i></div><div><i><b>(&#39;all&#39;,
&#39;particle_velocity_x&#39;=
)</b></i></div><div><i><b>(&#39;all&#39;, &#39;particle_velocity_y&#39;)
</b=
></i></div><div><i>(&#39;all&#39;, &#39;particle_velocity_z&#39;)
</i></div>=
<div><i>(&#39;io&#39;, &#39;particle_extra_field_1&#
39;)</i></div><div><i>(=
&#39;io&#39;, &#39;particle_extra_field_2&#39;)</i></div><div><i>(&#39;
io&#=
39;, &#39;particle_extra_field_3&#39;)</i></div><div><i>(&#39;io&#39;,
&#39=
;particle_extra_field_4&#39;)</i></div><div><i>(&#39;io&#39;,
&#39;particle=
_extra_field_5&#39;)</i></div><div><i>(&#39;io&#39;,
&#39;particle_identifi=
er&#39;)</i></div><div><i>(&#39;io&#39;, &#39;particle_mass&#39;)</i></
div>=
<div><i>(&#39;io&#39;, &#39;particle_position_x&#39;)
</i></div><div><i>(&#3=
9;io&#39;, &#39;particle_position_y&#39;)</i></div><div><i>(&#39;io&#39;,
&=
#39;particle_position_z&#39;)</i></div><div><i>(&#39;io&#39;,
&#39;particle=
_refinement_level&#39;)</i></div><div><i>(&#39;io&#39;,
&#39;particle_veloc=
ity_x&#39;)</i></div><div><i>(&#39;io&#39;, &#39;particle_velocity_y&#39;)
<=
/i></div><div><i>(&#39;io&#39;, &#39;particle_velocity_z&#39;)
</i></div><di=
v><i>(&#39;ramses&#39;, &#39;Density&#39;)</i></div><
div><i>(&#39;ramses&#3=
9;, &#39;Metallicity&#39;)</i></div><div><i>(&#39;ramses&#39;,
&#39;Pressur=
e&#39;)</i></div><div><i>(&#39;ramses&#39;, &#39;var6&#39;)</i></div><div>
<=
i><b>(&#39;ramses&#39;, &#39;x-velocity&#39;)</b></i><
/div><div><i><b>(&#39=
;ramses&#39;, &#39;y-velocity&#39;)</b></i></div><div><i>(&#39;ramses&#39;
,=
 &#39;z-velocity&#39;) &quot;</i></div><div><br></div><div>So, I am
thinkin=
g that the highlighted fields in the type &#39;all&#39; could be used to
co=
mpute circular velocity [sqrt(particle_velocity_x^2+
pa<wbr>rticle_velocity_=
y^2)] and the radius [sqrt(particle_position_x^2+
pa<wbr>rticle_position_y^2=
)] for particles. And for gas, &#39;ramses&#39; fields could be used.
Howev=
er, I am not sure how to get the radius for the gas in this case. Would
thi=
s be a right approach at all to begin with?</div></div></div></div><
/div><s=
pan>
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*SK2*

*"**Claiming that something can move faster than light is a good
conversation-stopper in physics. People edge away from you in cocktail
parties; friends never return phone calls. You just don’t mess with Albert
Einstein.**"*

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[yt-users] Error in streamline plotting

Sushilkumar