text:
\section{Introduction}

A concordance of observations support a universe of dark matter (DM), but all concrete evidence for its existence is solely based upon its gravitational interactions \cite{concord1,concord2,wmap9}.  Direct detection experiments aim to rectify this by observing collisions between dark matter and target nuclei.  A host of experiments report no observation of such events, continuing to place more stringent limits on the interaction cross-section.  Yet, the DAMA/LIBRA experiment \cite{dama_libra} reports a statistically significant annual modulation in its detector which could be attributed to the relative motion of the detector through the galaxy's dark matter halo. Furthermore, the CoGeNT  experiment \cite{cogent1} reports  signals above background in its detector which, if due to dark matter, would be consistent with the apparent signal from DAMA/LIBRA.  If these results are due to DM interactions, they occupy
a region of parameter space that has been seemingly ruled out by the CDMS-II \cite{cdmsii_ge} and XENON100 \cite{xe100} experiments.   To reconcile results from DAMA with null results from other experiments, the notion that DM could interact through inelastic channels has been proposed \cite{idm_tuckersmith,idm_chang,idm_marchrussell}.  By fine tuning the inelastic interactions, these models can simultaneously accommodate seemingly conflicting experimental results.

A natural way to incorporate inelastic interactions into a model is to allow DM to be composite, rather than point-like \cite{feng_hiddendm,kaplan_da1,cidm_alves,quirky,formfactor_dm,kaplan_da2,cline_da,kouvaris,wallemacq,cline_strong}.  To create composite particles in a dark sector, modelers introduce a new dark gauge group which results in a binding force among the composite's constituents.  The simplest gauge group is $U(1)$ \cite{feng_hiddendm,kaplan_da1,formfactor_dm,kaplan_da2,cline_da,wallemacq,cline_strong}.
If the symmetry is unbroken, then the dark photon is massless and can kinetically mix with the Standard Model (SM) photon.  In such models, the particles can effectively couple to the SM photon thereby acquiring a fractional electric charge  \cite{holdom}.  This permits the existence of dark atoms which are overall electrically neutral, but made of constituents with electric millicharge \cite{cline_da,wallemacq,cline_strong}.

The dark atoms form bound hydrogenic states under the exchange of dark photons, yet their tiny coupling to SM photons opens the possibility that these dark atoms can be probed with SM electromagnetism.  We will explore this possibility in what follows.  As the dark atoms are electrically neutral, they are essentially invisible to low energy photons.  However, for photons which are near the threshold energy needed to transition the dark atom to an excited state, an electromagnetic wave can resolve the charge distribution within the atom.  Considering dark matter as a bulk medium, the interaction between dark matter and light can be characterized in terms of an electric susceptibility and index of refraction \cite{loudon}.   For photon energies below the transition energy $\omega \ll \omega_0$, the medium will rather generically exhibit dispersion quadratic in the photon energy $n(\omega) \approx 1 + A + B\omega^2$ for constants $A$ and $B$.
Indeed, this is the expected form for the refractive index  from the classical Lorentz model for dielectrics \cite{lorentz}.  Furthermore, this form extends to the realm of particle physics. Combining Fermi's generalized index of refraction formula \cite{fermi} with the low-energy theorems governing the forward scattering amplitude of photons on point-like particles \cite{ggt,low,gg,g} yields the same structure for the refractive index.

The refractive index for various particulate DM models was considered previously in Ref.~\cite{dm_n}.  In that work, the neutral DM candidate coupled to massive charged particles which interacted with photons.  The process occurred at the one-loop level in perturbation theory and was, thus, highly suppressed resulting in an immeasurable index.  In the case of millicharged dark atoms, the photons can couple directly to the constituents of the DM candidate with measurable consequence.  The dispersive term in the index of refraction can be constrained by astrophysical observation.  If a broadband pulse of light is emitted over a short timescale from an astrophysical object such as the Crab Pulsar or a gamma-ray burst \cite{schaefer}, then a dispersive medium of dark atoms creates a time delay between higher and lower frequency photons.  Limits on a measured time delay can be used to constrain the dispersive term and, thus, the parameters that enter into models of atomic dark matter.

\section{Refractive index of dark atoms}

The atomic dark matter models in Refs.~\cite{cline_da,wallemacq,cline_strong} share a common dark and SM electromagnetic sector.  Two fermions $\psi_\mathbf{p}$ and $\psi_\mathbf{e}$ are charged under the unbroken gauge group $U(1)'$, coupling to the dark photon $\boldsymbol{\gamma}$ with opposite charges $\pm \mathbf{e}$.  [NB: The boldface type is meant to refer to the particles and couplings in the dark sector.]  Kinetic mixing between the dark and SM photons gives rise to an electric millicharge $\pm \epsilon e$ of the dark particles.  The dark ``proton" and ``electron" can form bound states under the dark Coulombic potential $V(r) =  -\boldsymbol{\alpha}/r$, where we define the dark fine structure constant $\boldsymbol{\alpha} := \mathbf{e}^2/ (4\pi)$, and the relative separation between the particles is $r$.   We can use non-relativistic quantum mechanics to describe this dark ``hydrogen", $\mathbf{H}$.  Without loss of generality, we assume $m_\mathbf{e}\le m_\mathbf{p}$ and define the reduced mass $m:= m_\mathbf{e} m_\mathbf{p}/(m_\mathbf{e}+m_\mathbf{p})$.  The relative momentum of the system is  $\mathbf{p} := m\dot{\mathbf{r}}=(m_\mathbf{p} \mathbf{p}_\mathbf{e}-m_\mathbf{e} \mathbf{p}_\mathbf{p})/(m_\mathbf{e} +m_\mathbf{p})$.    From these, we construct the Hamiltonian $H_0 := - \nabla^2/(2m) + V(r)$, which yields the usual  hydrogenic eigenstates $\psi_{n,\ell}$ and energy spectrum $E_n = - \boldsymbol{\alpha}^2 m/(2n^2)$ for quantum numbers $n =1,2,\dots,$ and $|\ell|\le n$. For large values of the dark fine structure constant $\boldsymbol{\alpha}\sim \mathcal{O}(1)$, the fine structure will  introduce significant corrections to the energy levels, and hyperfine structure will become relevant if $m_\mathbf{e}\sim m_\mathbf{p}$.  We will not consider these corrections in what follows.

Classically, a linear dielectric medium, such as  a dilute gas of dark atoms, will acquire a polarization when subjected to an external electric field.  The degree of polarization, or dipole moment per unit volume, can be characterized through the electric susceptibility $\mathbf{P} = \chi_e \mathbf{E}$.  From the susceptibility, we can compute the medium's index of refraction $n =\sqrt{1+\chi_e}$.  To compute the susceptibility of a dark-atom medium, we follow the semiclassical treatment in Ref.~\cite{loudon} in which a classical electromagnetic wave of frequency $\omega$ interacts with the quantum mechanical electric dipole moment of the dark atom $\pmb{\mathpzc{p}} := -\epsilon e \mathbf{r}$.  In the long wavelength limit, $\omega \ll \boldsymbol{\alpha} m =: \mathbf{a}_0^{-1}$, the spatial variation of the electric field is irrelevant, and we incorporate interactions between the wave and the dark atom by including in the Hamiltonian the time-dependent perturbation $H' =-\pmb{\mathpzc{p}} \cdot \mathbf{E}_0 \cos \omega t$.

The electromagnetic wave can induce transitions  between dark atomic energy states.  We argue that the bulk of the dark atoms exist in the ground state.  There are three main mechanisms by which the atoms can be excited beyond the ground state: dark atom self-interactions, absorption of dark photons,  or absorption of SM photons.    The existence of elliptical DM halos severely constrains the DM self-interaction cross section; from the limits in Ref.~\cite{MiraldaEscude:2000qt}, we find that the ratio of the DM self interaction to the dark atom's mass must be $\sigma/m_\mathbf{H} < 0.02$ cm$^2$/g.   These limits can be satisfied
either through tuning the model parameters or dilution of the dark atom component of DM.   For models which satisfy this constraint, we can estimate the mean free time between collisions for dark atoms in the Milky Way's galactic halo.  The mean free path can be estimated as $\lambda \sim (\sigma N)^{-1}$ where $N$ the number density of dark atoms; the number density is related to the DM mass density via $N = \rho/m_\mathbf{H}$.  Then the time between collisions is $t_\text{fp} \sim \lambda/v =  m_\mathbf{H} /(\sigma \rho v) $.  Taking as typical parameters the local dark matter density $\rho \sim 0.3$ GeV/cm$^3$ and $v\sim 200$ km/s, we find $t_\text{fp} \gtrsim 5 \times 10^{18}$ s; i.e., they are non-interacting.
Dark-atom absorption of dark photons also produce excited states.  The greatest energy density of dark radiation is found in the dark analog of the cosmic microwave background (CMB).  Viable models require the dark radiation to be slightly cooler than the CMB  \cite{adm_cosmo}, so these dark photons will not have sufficient energy to excite the dark atoms.  All that remains is the interaction with SM electromagnetic waves, which we discuss below.

We consider a dark atom in its ground state which can be excited by SM photons.  We  restrict our study to a two-state system, limiting the electromagnetic wave frequency to $\omega \lesssim \omega_0 := E_2-E_1$.  In the presence of the electromagnetic wave, the Hamiltonian for the dark atom is $H= H_0 + H'$, and a general state is $\Psi(t) = c_1(t) e^{-i E_1t} \psi_1+c_2(t) e^{-i E_2t} \psi_2$, with stationary eigenstates $\psi_{1,2}$.  Using the Schr\"odinger equation, we can develop coupled differential equations for the coefficients $c_1$ and $c_2$.  These equations must be amended to account for spontaneous emission of a dark photon from the excited state--a field theoretic result.  With this extra term proportional to the decay constant $\Gamma$, we have the equation for $c_2$
\begin{equation}
\frac{\mathrm{d}}{\mathrm{d}t} c_2(t) = -i \, (\pmb{\mathpzc{p}}_{21}\cdot \mathbf{E}_0) e^{i\omega_0t} \cos(\omega t) c_1 (t)   -\Gamma c_2(t)
\end{equation}
where $ \pmb{\mathpzc{p}}_{21} := \langle \psi_2 | \pmb{\mathpzc{p}}  | \psi_1  \rangle$ and $\Gamma=  \frac{2^7}{3^8}\boldsymbol{\alpha}^5 m$, adapted from atomic hydrogen \cite{loudon}.

We solve perturbatively for the coefficients $c_{j}(t) = c_{j}^{(0)}(t)+ c_{j}^{(1)}(t)+\cdots$  with initial conditions $c_1(0)=1$ and $c_2(0)=0$.  To determine the {\em linear} response of the atom to the field $E_0$, we only need the zeroth order approximation for $c_1 \approx 1$ and the first order approximation for $c_2$
\begin{equation}
c_2(t) \approx -\frac{1}{2} (\pmb{\mathpzc{p}}_{21}\cdot \mathbf{E}_0) \left[ \frac{e^{i(\omega_0 + \omega)t}}{\omega_0 + \omega - i \Gamma}+\frac{e^{i(\omega_0 - \omega)t}}{\omega_0 - \omega - i \Gamma }\right].
\end{equation}
The induced dipole moment for $\Psi$ is thus
\begin{equation}
\pmb{\mathpzc{p}}(t) = -\epsilon e \langle \Psi(t) | \mathbf{r} | \Psi(t) \rangle = -2\epsilon e\,  \mathrm{Re} [ \mathbf{r}_{12} c_1^*c_2 e^{-i \omega_0 t}].
\end{equation}
We note that the polarization $P(t)$ will be the product of the average induced dipole moment in the direction of $\mathbf{E}_0$ and the number density $N$.  Averaging over the relative orientation between $\mathbf{r}_{12}$ and $\mathbf{E}_0$,   the susceptibility is
\begin{equation}
\chi_e = N\pi\frac{2^{18} }{3^{11}}  \frac{\epsilon^2 \alpha }{\boldsymbol{\alpha}^2 m^2}\frac{\omega_0}{\omega_0^2 -(\omega+i\Gamma)^2}.
\end{equation}

Given that the DM medium is weakly interacting and dilute, $\chi_e$ is nearly zero.  As such we can approximate the index of refraction as $n \approx 1 +\frac{1}{2} \chi_e$.  For frequencies below the transition energy $\omega < \omega_0$, the index of refraction exhibits normal dispersion; that is, $n(\omega)$ increases with $\omega$.  In fact, for $\omega \ll \omega_0$, the dispersion is quadratic in frequency
\begin{equation}
\mathrm{Re}(n) \approx 1  +  N\pi\frac{2^{20} }{3^{12}}  \frac{\epsilon^2 \alpha }{\boldsymbol{\alpha}^4 m^3}\left( 1 + \frac{\omega^2}{\omega_0^2}\right) ,
\end{equation}
neglecting the small term proportional to $\Gamma^2$.

\section{Limits from the Crab Pulsar}

As a broadband pulse of electromagnetic radiation travels through a dispersive medium, the pulse shape spatially broadens since the phase speed of each component wave is frequency dependent.  For a medium which is normally dispersive, higher frequency components of the pulse will lag the lower frequency components.  Over large distances, a time lag can accrue between these two components.  For a dispersive medium of atomic DM, the time lag between simultaneously emitted waves of frequency $\omega_\text{hi}$ and $\omega_\text{lo}$ traveling over a baseline $\ell$  is
\begin{equation}
\tau \approx \ell N\pi\frac{2^{20} }{3^{12}}  \frac{\epsilon^2 \alpha }{\boldsymbol{\alpha}^4 m^3}\left( \frac{\omega_\text{hi}^2 -\omega_\text{lo}^2}{\omega_0^2}\right), \label{time_lag}
\end{equation}
assuming $\omega_\text{hi}\ll \omega_0$.

\begin{figure}[t]
\includegraphics[width=8.6cm]{fig1.pdf}
\caption{(Color online) Constraint on the electric millicharge $|\epsilon| e$ of the dark electron and proton from the Crab Pulsar dispersion limits with $\boldsymbol{\alpha}=1$.  The dashed (red) curve has $m_\mathbf{p}=100$ keV; the dotted (blue) curve has $m_\mathbf{p}=10$ keV; the dot-dashed (green) curve has $m_\mathbf{p}=1$ keV; and the solid (black) curve has $m_\mathbf{p}=100$ eV.  The parameter space above each curve is excluded by the data.\label{fig1}}
\end{figure}

The frequency dependence of the speed of light has been severely constrained in the optical spectrum from the observation of radiation coming from the Crab Pulsar.  The phase difference between 0.35 and 0.55 $\mu$m radiation was determined to be less than 10 $\mu$s \cite{crab_pulsar}.  Since the pulsar is 2 kpc from the Earth, this provides a stringent limit on the ratio $\tau/\ell \approx 5 \times 10^{-17}$.    We will assume that the entirety of dark matter in the galactic halo is atomic DM, and to yield the most conservative constraints on the properties of dark atoms, we will assume that any dispersive effects suffered by light are due exclusively to the dispersion from atomic DM.  Since our limits are only valid for $\omega \ll \omega_0$, the high frequency observation places bounds on the product of the dark fine-structure constant and the system's reduced mass $\boldsymbol{\alpha}^2 m \gg \frac{8}{3} \omega_\text{hi} = 9.5$ eV.  We will assume the local DM mass density to be $\rho = 0.3$ GeV/cm$^3$, and then the DM number density is $N = \rho/m_\mathbf{H}$ where $m_\mathbf{H} = m_\mathbf{p} + m_\mathbf{e} -\frac{1}{2}\boldsymbol{\alpha}^2 m$.

The most severe constraints on the properties of the dark atoms will come from photons whose energies are close to the transition energy, i.e., $\omega_\text{hi} \sim \omega_0$.  In the case of the Crab Pulsar, we have $\omega_\text{hi} =3.5$ eV, which limits the product $\boldsymbol{\alpha}^2 m$ to be on the order of tens of electronvolts.  For $\boldsymbol{\alpha} =1$, the most massive dark atom that we can meaningfully constrain has a dark proton mass $m_\mathbf{p} = 1.0 $ MeV; then for a dark electron mass of 9.5 eV, the electric millicharge of these particles satisfies $\epsilon < 0.84$.  For smaller dark proton masses, there is a broader range of dark electron masses that leads to meaningful constraints on the millicharge, Fig.~\ref{fig1}.  For a dark proton mass of 100 keV, a dark electron mass of $10$ eV provides the most stringent constraint on the millicharge, $|\epsilon| < 0.3$.  Limits improve with lighter atoms.  For example, a dark atom with $m_\mathbf{p} = 100$ eV and $m_\mathbf{e} = 20$ eV results in the constraint $|\epsilon|< 0.04$.

The dark atomic masses constrained by dispersion are much smaller than those of the dark matter candidates in Ref.~\cite{cline_da}, $\sim 6$ GeV, and Ref.~\cite{wallemacq}, $\sim 650$ GeV.  Indeed, the region of parameter space which we exclude is already ruled out by the self-interaction limits found in Ref.~\cite{MiraldaEscude:2000qt}.
Furthermore, stringent limits on the existence of millicharge particles, cf.~Refs.~\cite{davidson,Vogel:2013raa}, would rule out the dark protons and electrons constrained by our dispersion limits.

\section{Potential limits from GRBs}

Observations of the Crab pulsar place severe constraints upon the dispersive nature of the interstellar medium in the Milky Way,
yet these constraints are only relevant for a narrow band of the electromagnetic spectrum.  Even more severe constraints can be derived from distant sources like gamma ray bursts (GRBs), and these constraints span a much broader spectral range.
GRBs produce an intense burst of high-energy photons on a short time scale which can be viewed over cosmological distances, increasing the effective baseline, $\ell$ in   Eq.~(\ref{time_lag}), between the source and observer.  The high-energy photons from GRBs, upwards of 100 GeV, have the potential to constrain composite millicharged dark matter of greater mass, and the associated optical, infrared, and radio afterglow allow for their use in broadband observations.  The high energy photons from distant GRBs have already been used to place lower bounds on the scale at which Lorentz-invariance violating effects could modify the photon's dispersion relation \cite{AmelinoCamelia:1997gz,ellis,Boggs:2003kxa,Ellis:2005wr,jacobpiran,ellis2,Ellis:2009yx,AmelinoCamelia:2009pg,Vasileiou:2013vra}.  Along similar lines, we will consider how the (non-)observation of dispersion, attributable to dark matter, impacts the properties of composite dark matter.

Relative to the Crab pulsar, using GRBs for dispersion studies has two drawbacks:  the intergalactic DM density is much smaller and the temporal profile of the source is not known.  With regards to the DM density, the Crab pulsar is within the Milky Way where the dark matter halo density is relatively large.  For distant GRBs, the average DM density is $\rho \simeq 1.20\times 10^{-6}$ GeV/cm$^3$\cite{wmap9}, a factor of $10^5$ smaller than our local density.
In terms of timing resolution, the pulsar is well suited for dispersion studies because its regular rotational period means the temporal profile of light emitted from these objects is well known.  GRBs do not share this feature; the spectra of the bursts  \cite{Gruber:2014iza} and their lower frequency afterglows \cite{Meszaros:1996sv,Cenko:2010cg,Zaninoni:2013hca}  are varied.  Since dispersion measurements rely on temporal knowledge of the emission spectra, a single GRB event cannot yet be used to constrain DM properties.  But with a large number of GRB observations located at a variety of redshifts, it is expected that, statistically, random variations amongst the sources should wash out, and any real effects that indicate dispersion should survive.  The Fermi Gamma-Ray Space Telescope \cite{fermi_lat} is  dedicated to the task of gamma-ray observations, so that in the future, a sufficient number of GRBs may be used to provide meaningful constraints.  Despite the present dearth of data, we will estimate the possible reach of such a study based upon the observation of a single burst.

Since GRBs can be viewed at cosmological distances, the frequency-dependent time-lag accrued by simultaneously emitted pulses of light traveling through a dispersive medium of dark atoms requires modification due to the universe's expansion \cite{jacobpiran}.  First, the light-travel time between source and detector is dependent upon the redshift of the source and the local expansion rate.  Second, at redshift $z$ the number density of dark matter increases by a factor of $(1+z)^3$.  Finally, as we look into the past, the wavelength of light blue shifts relative to its value $\omega$ at the detector (at $z=0$). Incorporating these three factors, the time lag accrued between (detected) frequencies $\omega_\text{hi}$ and $\omega_\text{lo}$ simultaneously emitted from a source at redshift $z$ becomes
\begin{equation}
\tau \approx N\pi\frac{2^{20} }{3^{12}}  \frac{\epsilon^2 \alpha }{\boldsymbol{\alpha}^4 m^3}\left( \frac{\omega_\text{hi}^2 -\omega_\text{lo}^2}{\omega_0^2}\right) \int_0^z \frac{(1+z')^5 \mathrm{d}z'}{H(z')}
\end{equation}
where $N$ is the present-day DM number density and  the Hubble expansion rate at redshift $z'$ is $H(z') = H_0 \sqrt{(1+z')^3\Omega_M + \Omega_\Lambda}$.
The cosmological parameters determined through the combined analysis of WMAP nine-year data
in the $\Lambda$CDM model with  distance measurements from Type Ia supernovae (SNe) and with baryon acoustic oscillation
information from the distribution of galaxies can be found in Ref.~\cite{wmap9}. The Hubble constant
today is $H_0 = 69.32 \pm 0.80 \,\hbox{km/s/Mpc}$, whereas
the fraction of the energy density
in matter relative to the critical density today is $\Omega_M = 0.2865^{+0.0097}_{-0.0096}$ and
the corresponding fraction of the energy density
in the cosmological constant $\Lambda$ is
$\Omega_\Lambda = 0.7135^{+0.0095}_{-0.0096}$~\cite{wmap9}.

The maximum reach for idealized GRB constraints are derived from observations of the most distant events. There have been two GRB observations with confirmed redshift $z>8$:  GRB 090423 with $z=8.3\,$ \cite{Tanvir:2009zz} and GRB 090429B with $z=9.4$ \cite{Cucchiara:2011pj}.  We will use as our exemplar the observation of GRB 090423 because, in addition to the burst detection, the afterglow was observed down through the radio band \cite{grb090423_radio}.  The strength of the pulsar constraint relied on the fact that the detector's temporal resolution was $\sim 10 \mu$s.  This same resolution is possible for the Fermi Large Area Telescope which detects gamma rays from 20 MeV up to 300 GeV \cite{fermi_lat}; however, this resolution is likely not possible for the variety of ground based telescopes which observe the GRB afterglows.  For example, the integration times for the ground-based Gamma-Ray Burst Optical and Near-Infrared Detector are on the order of tens to hundreds of seconds \cite{grond}.  Longer integration time weakens the ability to constrain dispersion for large values of the dark fine-structure constant $\boldsymbol{\alpha}$, but meaningful constraints are realizable in the radio band. We estimate such constraints for GRB 090423 for a small value of $\boldsymbol{\alpha}$.

The most competitive limits arise whenever the observed high-frequency photons are near the threshold energy $\omega_\text{hi} \sim\omega_0$; however, we must be mindful that the wavelength blueshifts as we look into the past.  In order to not surpass the threshold energy at redshift $z$, we must limit the measured high frequency photons to $\omega_\text{hi} \sim (1+z)^{-1} \omega_0$.  Assuming this, along with a large separation between high and low frequency bands $\omega_\text{hi} \ll \omega_\text{lo}$, we find limits on the electric millicharge of the dark electron to be
\begin{equation}
\epsilon^2  \lesssim \frac{(1+z)^2\tau}{2\pi \alpha \rho }  {\boldsymbol{\alpha}^4m_\mathbf{H} m^3} \left[ \int_0^z \frac{(1+z')^5 \mathrm{d}z'}{H(z')}\right]^{-1}
\end{equation}
Consulting Ref.~\cite{grb090423_radio}, we find that the location of GRB090423 was observed by several radio telescopes but detection of the afterglow was only confirmed by the Plateau de Bure Interferometer \cite{GCN9273} (at 100 GHz) and the Very Large Array (VLA)\cite{grb090423_radio} (at 8.46 GHz).  These detections were separated by eight days, so they cannot provide a meaningful constraint.  What is needed is near simultaneous multi-band detection of the GRB; at best, we can make a reasonable estimate of the reach of such a detection.  We suppose that a high frequency observation is made by the VLA at 8.46 GHz while a lower frequency observation is made by another telescope.  Typical integration times for these telescopes are on the order of tens of minutes, but for our purposes, we suppose a somewhat optimistic integration time of 100 s.  Then, if the detection of the GRB can be established at 8.46 GHz and a lower frequency within this 100 s window, we find that this measurement could constrain the electric millicharge of a dark atom with masses $m_\mathbf{e} = m_\mathbf{p} = 1$ keV and $\boldsymbol{\alpha}=5\times10^{-4}$ to be $\epsilon \le 2.8\times 10^{-4}$.

This estimate is competitive with terrestrial constraints on the existence of millicharged particles derived from colliders.  For particle masses below 200 MeV, the SLAC electron beam-dump experiment \cite{Donnelly:1978ty,slac_ebd} limits the particle's millicharge to be $\epsilon \le 3\times 10^{-4}$ \cite{Davidson:1991si}.  On the other hand, millicharged particles with masses in the keV range would disrupt big-bang nucleosynthesis in the early universe; constraints upon the light degrees of freedom would preclude the existence of these millicharged particles \cite{Davidson:1991si}.

\section{Conclusion}

Dark matter models which consist of composite states under some unbroken $U(1)'$ gauge symmetry can explain possible DM signals in the DAMA/LIBRA and CoGeNT experiments that are seemingly inconsistent with the null results from the CDMS-II and XENON100 experiments.   In some models, the dark photon mixes with the standard model photon resulting in electric millicharges for the particles in the dark sector.    This interaction with the SM photon results in non-trivial optical properties for a dark-matter medium.  We computed the electric susceptibility of a medium of dark atoms and determined that such a medium is dispersive.  The dispersion can result in time lags between simultaneously emitted pulses of light of differing frequencies.

Using stringent limits on the (optical) frequency dependence of the speed of light from the Crab Pulsar, we are able to constrain the properties of a dark matter medium consisting of dark atoms.  For a dark fine structure constant $\boldsymbol{\alpha}=1$, we find that we can limit the electric millicharge of dark (electrons) protons to be less than the SM proton charge, $| \epsilon| \le 1$, for dark atom masses below 100 keV.  Millicharged particles in this mass range have been ruled out by collider searches and interact too strongly to be consistent with the dark matter haloes of elliptical galaxies.  GRBs yield more stringent constraints on the dispersion of the cosmos.  Given their brightness and broad spectral range, these objects are promising sources by which we can constrain millicharged atomic dark matter.  We estimate that observations of the radio afterglow could result in constraints on the electric millicharge of the dark electron and proton for masses in the keV range that are competitive with collider constraints; however, big-bang nucleosynthesis would rule out the existence of these light particles in the early universe.

The technique that we develop in this work, namely that cosmic dispersion can constrain dark atomic  properties, is applicable to other models of composite dark matter that have millicharged constituents.  At present, we know of no other models of composite dark matter with millicharged constituents.  Likely, this is due to parsimony; i.e., the composite system is bound under some broken gauge group so that charged constituents under a new $U(1)'$ gauge group would be superfluous.  However, the dark sector could be as complex as the Standard Model sector, and the constituents of the composite dark matter could indeed couple to dark photons, opening the possibility that they acquire an electric millicharge.  If this is the case, then dispersive constraints would impact the parameters of the composite dark matter model.

\section{ACKNOWLEDGMENTS}

AK acknowledges partial support during the completion of this work from the  Washington NASA Space Grant Consortium and  the University of Puget Sound.  DL thanks Bernie Bates for useful discussions on radio astronomy.

\bibliographystyle{ws-mpla}

redpajama_set_name: RedPajamaArXiv


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text:
How To Pee During The Red Carpet: 15 Answers To Questions You've Always Wondered About The Oscars
by Jordan Runtagh 2/27/2013
Like most of us, I've often fantasized about attending the grand glittering spectacle known as the Academy Awards. But tragically I've been held back by my total lack of acting skills, directing skills, or any film-related talent whatsoever. Yet one day out of the clear blue sky I was given the once in a lifetime opportunity to gain access Hollywood's ground zero. I was lucky, but getting the green-light was just the beginning. There were many many unexpected steps on the journey to the golden bald man. So if you ever find yourself married to Sandra Bullock and have to be her date to the Oscars, these are some logistics you will have to consider when turning your Oscar fantasy into a reality.
1. What The Hell Do You Wear?
"Who are you wearing?" You hear that phase uttered at least six thousand times on any given award ceremony pre-show. Obviously for a job like this, I knew that wardrobe was clutch. But really now, what does a 25-year-old dude who wears cowboy boots on the reg wear to the Oscars? I had no idea. With only two weeks to prep, I didn't have much time. Should I go to a bespoke tailor? A high-end designer store? Hire a professional shopper? What would George Clooney do? Then it hit me.
I put in a call to Men's Warehouse.
Soon I was allowing a man with a tape measure to grope me in the middle of a room full of nervous teenagers, really nervous grooms, and proud moms. Then a very nice lady explained to me why a cane would make me look like a creep. She asked me to choose between three seemingly identical starched white shirts. Which of these would Clooney take? I closed my eyes and prayed I had chosen correctly. I didn't want to look like my dad at his high school prom in 1973.
2. How Do You Get To California?
Unless you live locally, are very big on road tripping, or possess the ability to teleport, getting to the Oscars will require you to enter a tin-can filled with other people's morning breath and be launched towards the west coast at very high speeds. My tin-can left bright and early at 7 AM. I thought about taking a peek in First Class for celebrities, but I soon realized that no self respecting famous person would ever agree to a 7 o'clock flight.
3. How Do You Get Your Credentials?
The Oscars aren't just like your neighbors' 4th of July barbecue. You will not be able to Wedding Crashers your way into this thing. That's why I had to head over to pick up my security badges the morning before, otherwise I'd be stuck on the outside looking in, like that tattoo guy who used to be married to Sandra Bullock.
The Academy Awards take place at the newly renamed Dolby (formerly Kodak) Theater in the impressive Hollywood and Highland complex, just a few blocks from my hotel down the star-lined Hollywood Boulevard. The whole street is like a giant carnival midway with mechanical Gypsy fortune tellers, Egyptian throwbacks to the 1920s, and, of course, palm trees. Mannequins, wax museums and McDonalds fill the thoroughfare. I'm probably not the first one to note that Hollywood can sometime seem a trifle…fake. I hustle over the Hollywood Walk of Fame sidewalk. It's very long and filled with an insane number of really random no-namers. So if you're a celeb and you haven't got your name on a star already you should probably re-examime your life choices
Finally I see the red carpet site up ahead, smack in the middle of the closed-off road. It felt vaguely undignified to see such a high glam event in the prep stages. Like walking in on someone talking a shower or something. The 15-foot golden man standing at the end of the carpet is wrapped in protective Saran wrap and gaffers tape like a massive Edible Arrangement. Tech crew were running amok over the space. And the red carpet badly needed to be vacuumed. Plain clothed crew walk around wearing sheets of paper with famous names (Channing Tatum, Kelly Rowland) attached to them. I'm kind of surprised how small the whole affair is (about a short city block wide from start to finish). Scaffolding and camera cranes tower all around. It's not like you see on TV. In true Hollywood tradition, they know all the good angles to shoot.
I head in to the complex's Lowes hotel and wait in line to be photographed and get my badges. It's just like a glittery DMV, but full of really well-dressed people with cameras and tape recorders dangling around their necks. A few minutes later it's all official: I'm going to the Oscars.
4. How Do You Wear A Tuxedo?
Boom, it's the big day! Time to slam on some Beastie Boys, Abba and Wham, hit the shower and make yourself look sharp! But then it was time for another obstacle: Getting dressed.
One of the great myths about tuxedos is that it's a magic garment that instantly transforms you into James Bond the moment you put it on. Instead I look like a game show host. Factor in this weird cummerbund thing and I appear to be a game show host with a back problem. Cufflinks, studs, pocket squares, suspenders…There are far too many moving parts on a tuxedo. How do you figure out all out? I spend a great deal of breakfast looking up "tux tutorials" on youtube. I'm sure Clooney does the same thing on Oscar morning.
5. What Time Do You Get To The Oscars?
The Academy wants you to be in place by 2 PM (the carpet opens at 2:30), so I assumed I could just easily walk from my hotel like yesterday. Right? Wrong. Very very wrong.
6. How Do You Get To The Oscars?
How do you get to the Academy Awards? No, it's not practice practice practice. The formerly hoppin' tourist street now looked like some post apocalyptic disaster movie. Everything is eerily still and empty. Sidewalks are all barricaded with high chain-link fences. Imposing concrete cubes block the roads, and LAPD cops line every corner. The sound of choppers circling above is deafening, and I half expect a rope to drop and a SWAT team to slide down and take me. It's pretty scary.
Designated parking areas are assigned in various local hotels. I assumed I'd have an easier time on foot. I thought wrong. Policemen send me on a round-about route, many blocks out of my way. Even with my badges, I go through several security check points, medal detectors, and bag searches. But finally I'm in. And I'm hungry.
7. What Do You Eat At The Oscars?
Press gathered in a small alley just south of Hollywood Boulevard, and directly behind the Late Night With Jimmy Kimmel studios. Phalanxes of satellite trucks and RVs (known as "Star Wagons") fill the lots. The Academy doesn't cater for us press-folk, and sadly Wolfgang Puck's Oscar cake is off limits to us.
So we're kind of on our own in the way of food. Luckily our gracious VH1 crew order us a heap of burgers and fries from the iconic California chain, In-and-Out for our very own Oscar Noms. We chow down and head to the carpet. And that's where I rapidly discovered many questions and answers. Starting with…
8. How Do You Walk On The Red Carpet?
We've all been there: It's a super fancy occasion so you bust our the shiny patent leather Buster Brown's you've only worn once to your cousin's wedding three years ago. You're feeling slick and good, but those smooth soles are out for blood and you fall right on your face. Yes, fancy shoes are slippery and pose quite the hazard. How do you keep yourself from falling flat on your face during Hollywood's biggest night? Our very own Janell Snowden gave me the answer: duct taping the soles of your shoes. Brilliant! I do the same, and soon I can move without fear.
9. Where Do You Stand On The Red Carpet?
Space is obviously tight at an event like this, and it required some serious musical chairs to get a spot for little old me. Three-tiered bleachers line the edge of the carpet, with "TV personalities" in the front row, producers and tech crew one step up, and camera men with the good birds' eye view on top. I had a small 2×3 rectangle marked off for me, and let me tell you; You become VERY territorial over that 2×3 space. A stray cord or misplaced water bottle takes on the seriousness of an invasion.
Looking around at some of the other larger media outlets, I began to feel trickles of "spot envy" creeping in. But then Extra correspondent Mario Lopez took the spot next to me, so I realized it couldn't have been too bad. What's good enough for Slater is good enough for me. I would have wished for Maria Menounos, but this isn't a perfect world.
10. What Do You Do If You Don't Know Who A Celebrity Is?
2:30. Show time! The press and crews are poised and ready for action, and bodies start streaming down the red carpet. It's very exciting, right!? Ehhh, not so much. In the same way that it's kinda lame to show up at a party right when it starts, most of the big names are waiting to make their big entrance. So for the first hour, you're stuck with folks like second producer of the best foreign animated short. What do you do when you're fishing for interviews and you're face to face with a "celebrity" who you've never seen before in your life? Well thankfully their publicists march out in front of them, holding pieces of paper bearing their names and what they've done to get them to the Oscars. Yeah, it's gotta be a little embarrassing, but much less embarrassing than a potential interviewee catching you Wikipedia-ing them on your phone.
Soon enough the big guns start trickling in. They take a minute to get down to my part of the carpet, but you know they're coming because of the crowd's screams.
11. How Loud Does It Get On The Red Carpet?
Think of a basketball game after the final buzzer. Or a baseball game after a home run. Or the Super Bowl when it's all over and the Quaterback is saying he wants to go to Disney World. Yeah, it's that loud. A frenzy is starting to take over. I'm so excited that I could wet my pants! But then a thought hit me. One that had never cropped up during my wild Oscar fantasies…
12. What Do You Do If You Have To Pee On The Red Carpet?
Despite only being February, it was pretty hot on Oscar Day. I had downed quite a few water bottles in order to stave off the ultimate humiliation: Fainting on the red carpet. But that brought with it it's own issues, and now I really had to go to the bathroom. What was I going to do!? Cameras to the left of me, Mario Lopez to my right, red carpet dead ahead? I was trapped! For a while I tried to just suck it up and deal with it, but realizing that holding my knees together in pain would severely compromise my reporting skills, I flagged down a security guy. He lead me down a small path behind the bleachers, and down an alleyway with portapotties. No, not glittering Hollywood portapotties— just regular ones.
13. Which Celebrities Looked Way Better In Person?
Pretty soon things got into full swing. Something I hadn't realized was how constant the flow of people was going to be. It wasn't just couples going one by one like a damn square dance. This is a mad dash filled with the entertainment elite! The carpet was so full that it takes a minute to realize that Steven Spielberg, Ang Lee, and Tom Hooper are ALL standing directly in front of you. There's just too much going on. But that being said, a few faces stood out as being strikingly gorgeous in person.
Clooney, Keibler, Kidman, Urban, Bullock, Affleck. Too much, does not compute.
Jessica Chastain is pure old school Hollywood glamour, and she got mucho bonus points for hugging pretty much every reporter she spoke to, even if they had just met. Maybe it's an old trick, but it worked on me. Plus her gorgeous hair bounced around like a dang Herbal Essences commercial.
It's no surprise that Jennifer Lawrence can really turn it on for the red carpet. Never has someone so attractive been so approachable. AND she won an Oscar a few hours later! Why must you have it all, J-Law?
And of course Harvey Weinstein looks good in anything.
14. Was Anne Hathaway's Alleged "Wardrobe Malfunction" Really That Bad In Person?
Ehh, not really.
15. Does George Clooney Shop At The Men's Warehouse?
Hard to tell, but our tuxes do look pretty similar…
[Photo: VH1]
Jordan Runtagh
VH1 Music Editor + Seltzer Enthusiast
@jordanruntagh
Tags: Anne HathawayJennifer Lawrence

redpajama_set_name: RedPajamaCommonCrawl


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Why Japan Is the Best Life Sciences Market in the World. Period.
Ask just about anyone about what the best, fastest-growing market in their specific sector is, and more often than on, you will run into the BRICs at some stage. But in the pharmaceutical and medical device space, there is one brightly shining, yet often overlooked, star – Japan.
At first sight, this may be surprising, since much of the headline news about Japan and the Japanese economy has not been positive for some time. There have been plenty of reasons - aging and shrinking population (in this regard, Japan is simply spearheading the trend that many other countries are going to experience, only a bit later), deflationary for more than a decade, new challengers throughout Asia, strong yen hitting exports, you name it.
However, dig deeper, and you will see that Japan continues to be a success story and a great market and leader in many industries. And, it is still the economy #3 globally, remember.
So what led Ira Wolf from PhRMA to declare "For foreign [drug] companies, it's the best market in the world right now?" The answer is: the "emerging-market" growth rates (12-31%) that multinational drug firms enjoy in Japan.
Drug Lags? No More.
Until very recently, Japan's Life Sciences market was, for many foreign manufacturers, characterized by the word "lag". The way the regulatory system worked caused major delays in the approval of drugs and medical devices in Japan. As a result, new products reached the Japanese market a lot later compared to Europe or the US. This also discouraged many manufacturers to actually try and get their devices or medicines approved in the first place. For new drugs, for instance, the total review time in the standard review process used to be well over 20 months.
It was PMDA (Japan's Pharmaceuticals and Medical Devices Agency), effectively a government body, that was tasked with the major overhaul of the Japanese system of drug approval, payment and administration (remember, PMDA has a much wider role in the whole health system in Japan compared with FDA or EMA). And their efforts are now bringing fruit.
Approval times have been vastly shortened and, as a result, the existing lags were greatly reduced. In addition, fewer expensive and cumbersome trials, often duplicating those carried out elsewhere, are now needed.
Among other things, the drug pricing system in Japan came under review. Prices of new drugs used to be lowered every two years (on average 6.5% last year). Under the new model, currently, in pilot, they may now be maintained through the life of the patent. This means a major impetus for research and development (R&D) in Japan. Among other recent achievements of PMDA, the goal of 30% of the drugs by volume to be generics has been already almost attained. Last but not least, PMDA created a Science Board composed of outside experts designed to improve its rulings on new technologies.
To illustrate the progress, compare how PMDA was able to reduce the review times for new drugs (priority reviews and standard reviews), and increase the number of approved applications.
Source: PMDA Annual Report 2011
Japanese Companies Go Global
All this has also helped the Japanese drug manufacturers thrive and increasingly expand internationally. While it has become harder to compete at home with the global big drug companies, they have used their cash to go on an acquisition spree. It is not too long since Takeda acquired Swiss Nycomed ($14B) or Millennium ($9B), Astellas paid $4B for OSI, or Daiichi Sankyo bought India's Ranbaxy for $4.6B. Some of the Japanese drug companies have moved their global R&D hubs to America. But most Japanese firms have not gone fully global yet: majority of their revenues still comes from home. Perhaps another proof of the attractiveness of the Japanese market.
We have spoken about what it takes to succeed on the Japanese pharmaceutical market at the Life Sciences Business Round Table, expertly moderated by Clio Schils, at the recent Localization World conference in Singapore. We will put Japan and Asia in the global context at the upcoming Round Table during the Localization World London, where we will speak about the regional differences between North America, Europe, and Asia in the context of Life Sciences translations, and the way companies from each region get their products ready or approved for local markets. See you in London!
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Davidson, you might recall, made his debut on the mound against the Rangers at Globe Life Park on June 29. He pitched a scoreless eighth and struck out Rougned Odor. He later pitched two other scoreless innings of relief during the season.
He was a first round pick in 2009 by the Arizona Diamondbacks.


Excerpt: It was a very well-designed package which included an added attraction of visiting the relatively un-explored destination of Hanoi, Vietnam over a period of 1 week.
Indian Paint & Coating Association has been a pioneer in taking delegations to various coating shows around the world. During the past few years, IPCA has taken delegations to China Coat, Vietnam, Russia and South Korea. This year yet again IPCA took a delegation for China Coat 2018, held at Guangzhou from 4th – 6th December 2018.
It was a very well-designed package which included an added attraction of visiting the relatively un-explored destination of Hanoi, Vietnam over a period of 1 week. The hotels were selected carefully considering the convenience to delegates. They were located in prime areas with close proximity to famous attractions. Surely visits to the major sightseeing locations and all the meals were included in the package. This well-designed package was a delight for the 55 strong delegation with a diverse representation of delegates from various parts of India. The group had members from all over India such as Delhi, Punjab, Haryana, Uttar Pradesh, Madhya Pradesh, Chhattisgarh, Maharashtra, Gujarat, and Karnataka.
IPCA organized direct flights from 3 centres New Delhi, Mumbai and Bangalore. All the delegates assembled together at Bangkok Airport to proceed to Hanoi, Vietnam. The place is rich in natural beauty with an amazing culture. It was nice to see a blend of tradition and modern culture at the Ionah show in Hanoi. A day long expedition to Halong Bay, a cruise ride with lunch served in the backdrop of limestone mountains and Dau Go Caves were really fun.
The delegates visited the Bai Dinh Pagoda, the largest Buddhist temple in Asia, and were amazed at the artistic creation of the Buddha Statues. The Trang An Grottoes tour is an amazing sight of majestic limestone massifs rising out of rice paddy fields over an area of 20 Sq. Kms. To take a serene ride in a canoe with sound of river water is one of the most peaceful experiences.
Having experienced the peaceful Vietnamese culture, the group proceeded to Guangzhou, reaching a day prior to the exhibition, the delegates enjoyed the day by relaxing & shopping at Beijing Lou which was just 500 meters away from the Hotel Landmark Canton where the group was staying.
Next day the delegates reached the exhibition grounds at 09.15 am as the hotel was barely 3.5 Kms away. Even though there was a huge crowd the entry for the IPCA delegation was smooth with all delegates been provided with personalized VIP badges to the coating show.
The delegates were served working lunches during all days of the show so that they can remain charged up to tackle the huge quest for knowledge. It was great to see people rushing from one meeting to another. Also the delegates were helping each-other in identifying potential booths for co delegates. The evenings were reserved for luxurious dinners at exotic Indian restaurants and a beautiful cruise on the pearl river, watching the amazing lights on the banks.
China is a fascinating place to travel. And if a group of colorful people from various parts of India are together then the trip becomes memorable. The group returned with pleasant memories of the trip with a hope of profitable returns from their meetings and the knowledge of latest technologies gathered from China Coat.


DES MOINES — For the third time, the Legislature has approved a resolution that would give voters the opportunity to adopt an amendment to the Iowa Constitution providing Iowans with the right to keep and bear arms.
Senate Joint Resolution 18 was approved Wednesday 33-16 in the Senate and 53-46 in the House, putting it on course to eventually be submitted to voters.
Before then, the resolution must be approved by the next General Assembly, which convenes in 2021, and then would be submitted to voters as early as 2022.
Legislators took up the issue again because the Iowa Secretary of State's Office failed to meet a notification requirement, forcing the amendment process to start over.
Like the outcome, there was little new in the debate.
The amendment would protect that freedom against potential future laws or executive orders from the federal government, said Sen. Brad Zaun, R-Urbandale. U.S. Constitution Second Amendment rights "have been eroded through many years," he added.
However, Democrats didn't think it was that simple. They argued the amendment would not only make passage of future gun regulations difficult, but also could make current regulations vulnerable.
"This creates a lot of unknown possibilities," said Sen. Tony Bisignano, D-Des Moines.
Democrats warned of the potential for legal challenges to current state regulations like prohibiting felons and domestic abusers from owning guns. They said, under the amendment, someone could challenge any of those regulations already on the books, and the courts may strike them down because of the strict scrutiny requirement.
Windschitl rejected the concerns, pointing out such challenges could be made today.
In both chambers, attempts to replace the wording of the state amendment with the actual language of the Second Amendment failed — on a party-line vote in the Senate, but in the House with Rep. Andy McKean, R-Anamosa, joining Democrats.
"I, too, revere the Second Amendment," McKean said. Although he supported joining 44 states that have Second Amendment language in their constitutions, he strongly opposed the inclusion of the "strict scrutiny" language.
"I have strong reservations about forcing judges to apply strict scrutiny to any and all gun laws," he said.
Only three states have that language. In recent years, eight states — six red states and two blue states, McKean said — have rejected it.
He also warned voters might reject the amendment because of the strict scrutiny standard.
"Iowans won't stand for that," said Rep. Mary Mascher, D-Iowa City. And if voters reject the amendment because of the strict scrutiny clause, she asserted, Windschitl will have endangered Iowans' gun rights.
Click Here to read the entire article written by James Lynch.


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'Guardians of the Galaxy' director James Gunn passed on a DC movie
Marvel's Guardians of the Galaxy director James Gunn has seen a lot of success with that franchise, but could he be bringing his skills over to DC one day?
According to Gunn, he's already been given the opportunity to direct a DC movie but decided not to for whatever reason. It sounds like he'd be open to it in the future though. Check out a recent exchange he had with a fan on Twitter below.
I've been given the opportunity. But who knows. Maybe?
— James Gunn (@JamesGunn) May 31, 2018
Do you think Gunn would be a good fit for a DC movie? Which one? Let me know in the comments below.


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Drako - The Juice
BROKEN? 18,715 views
Uploaded March 04, 2019
STREAM / DOWNLOAD: https://fanlink.to/drako-fullyloaded
***Catch Drako on The Slimeball Tour with Yung Nudy starting March 28th!
You are now watching the official video for "The Juice" by Drako, from the mixtape Fully Loaded, available worldwide via Babygrande Records. Video directed by GT Films Productions. Track produced by Lil Voe on the Beat & Dirty D.
Since emerging on the scene, Drako has received a tremendous amount of press and radio coverage and his tracks "Racks On Me," "Count It Up," and "Watch Me Do It" have accumulated over 7 million streams on Spotify alone. The Atlanta artist has recently collaborated with Lil Baby, Moneybagg Yo, Quando Rondo, and Yung Bans. Today, Drako has shared the official video for the standout track "The Juice," from his debut mixtape Fully Loaded. "The Juice," which was shot and directed by GT Films Productions showcases Drako's lavish taste and undeniable drip. The release of the video also coincides with Drako announcing that he is joining Young Nudy on a nationwide tour which kicks off in March. Drako will also be performing at the 2019 SXSW Music Festival in Austin, TX.
For more info on Drako, please visit:
https://www.instagram.com/real_drako/
https://www.twitter.com/drakosquad
https://www.facebook.com/drako404/
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